Author name code: wang-jingxiu
ADS astronomy entries on 2022-09-14
=author:"Wang, Jing-Xiu" OR =author:"Wang, J.-X." OR =author:"Wang, J.X." 
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Title: Characterization of Kepler targets based on medium-resolution
    LAMOST spectra analyzed with ROTFIT
Authors: Frasca, A.; Molenda-Żakowicz, J.; Alonso-Santiago, J.;
   Catanzaro, G.; De Cat, P.; Fu, J. N.; Zong, W.; Wang, J. X.; Cang,
   T.; Wang, J. T.
Bibcode: 2022A&A...664A..78F
Altcode: 2022arXiv220504757F
  <BR /> Aims: In this work we present the results of our analysis of 16
  300 medium-resolution LAMOST spectra of late-type stars in the Kepler
  field with the aim of determining the stellar parameters, activity
  level, lithium atmospheric content, and binarity. <BR /> Methods: We
  have used a version of the code ROTFIT specifically developed for the
  LAMOST medium-resolution spectra to determine stellar parameters via
  the adoption of a grid of spectra of real stars. We provide a catalog
  with the atmospheric parameters (T<SUB>eff</SUB>, log g, and [Fe/H]),
  radial velocity (RV), and projected rotation velocity (v sin i). For
  cool stars (T<SUB>eff</SUB> ≤ 6500 K), we also calculated the Ha
  and Li Iλ6708 equivalent width, which are important indicators of
  chromospheric activity and evolutionary stage, respectively. <BR />
  Results: From the sample of 16 300 spectra, we have derived the RV and
  atmospheric parameters for 14 300 spectra of 7443 stars. Literature
  data (mainly from high- or medium-resolution spectra) were used for
  a quality control of the results and to assess the accuracy of the
  derived parameters. The T<SUB>eff</SUB> and log g values are in good
  agreement with the literature, although their distribution displays
  some clustering effects, which may be the result of the nonuniform
  distribution of the templates in the parameter space. The most relevant
  differences are found for [Fe/H], which appears to be overestimated
  for metal-poor stars; this overestimation is also likely due to the
  template grid. We propose a relation to correct the [Fe/H] values
  derived with ROTFIT. We were able to identify interesting objects,
  such as double-lined binaries, stars with variable RVs, lithium-rich
  giants, and emission-line objects. Based on the Hα flux, we found
  327 active stars. We were able to detect the Li Iλ6708 line and
  measure its equivalent width for 1657 stars, both giants and stars
  on the main sequence. Regarding the latter, we performed a discrete
  age classification based on the atmospheric lithium abundance and the
  upper envelopes of a few open clusters. Among the giants, we found 195
  Li-rich stars, 161 of which are reported here for the first time. No
  relationship is found between stellar rotation and lithium abundance,
  which allows us to rule out merger scenarios as the predominant
  explanation of the enrichment of Li in our sample. The fraction of
  Li-rich giants, ≈ 4%, is higher than expected. <P />Full Tables C.2,
  C.3, 2, 3, and 4 are only available at the CDS via anonymous ftp to
  <A href="http://cdsarc.u-strasbg.fr">cdsarc.u-strasbg.fr</A>
  (ftp://130.79.128.5) or via <A
  href="http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/664/A78">http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/664/A78</A>

Title: The Nonuniformity of Poleward Flux Transport on the Solar
Surface: A Statistical Method Applied to Solar Cycles 21-24
Authors: Wang, Zi-Fan; Jiang, Jie; Wang, Jing-Xiu
Bibcode: 2022ApJ...930...84W
Altcode: 2022arXiv220316119W
  The poleward migration of the active regions' magnetic flux on the solar
  surface plays an important role in the development of the large-scale
  field development, especially the polar-field reversal, which is a
  key process in the Babcock-Leighton-type solar dynamos. The poleward
  flux transport is nonuniform, centered around poleward surges as
  suggested by previous observations. The strong, long-lasting surges are
  related to activity complexes, and often result in violent polar-field
  reversal. However, the nonuniformity of poleward flux transport has
  not been evaluated quantitatively. We propose a statistical method
  to analyze the poleward flux transport during solar cycles 21-24
  by considering the frequency distributions of the magnetic field
  at latitudes of poleward surges occurring during solar cycles. The
  nonuniformity is quantified as the kurtosis statistics representing
  the tailedness of the distributions. We test the method on results
  of surface flux transport simulations, and apply it to WSO, National
  Solar Observatory, MWO, and HMI data. We confirm that the poleward
  surges are of significance during solar cycles 21-24 in general. The
  kurtosis within a solar cycle is affected by different latitudes of the
  magnetic field and different data sources. The southern hemisphere of
  cycle 24 exhibits the largest kurtosis, agreeing with the super-surge
  concept from previous work. The significant nonuniformity of poleward
  flux transport originates from the nonrandomness of active regions,
  which favors the activity complexes as the origin of poleward surges.

Title: VizieR Online Data Catalog: Kepler targets class based on
    LAMOST spectra (Frasca+, 2022)
Authors: Frasca, A.; Molenda-Zakowicz, J.; Alonso-Santiago, J.;
   Catanzaro, G.; De Cat, P.; Fu, J. N.; Zong, W.; Wang, J. X.; Cang,
   T.; Wang, J. T.
Bibcode: 2022yCat..36640078F
Altcode:
  Spectral type, average atmospheric parameters (Teff, logg, and [Fe/H]),
  radial velocity (RV) and projected rotational velocity (vsini) are
  quoted in Table 2 for 7443 stars. <P />Table 3 reports the H-alpha
  equivalent width and flux at the stellar surface for 327 targets. <P
  />Table 4 reports the LiI-6708 equivalent width and lithium abundance
  for 1657 targets. <P />(5 data files).

Title: Response of the Fe Kα line emission to the X-ray continuum
    variability in the changing-look active galactic nucleus NGC 1566
Authors: Liang, W. C.; Shu, X. W.; Wang, J. X.; Tan, Y.; Zhang, W. J.;
   Sun, L. M.; Jiang, N.; Dou, L. M.
Bibcode: 2022JHEAp..33...20L
Altcode: 2022arXiv220111050L
  NGC 1566 is a changing look AGN known to exhibit recurrent X-ray
  outbursts with each lasting for several years. The most recent X-ray
  outburst is observed on 2018, with a substantial increase of 2-10 keV
  flux by a factor of ∼24 than the historical minimum. We re-analyze
  the XMM-Newton and NuSTAR observations covering the pre-outburst,
  outburst and post-outburst epochs, and confirm the discovery of the
  broad feature in the ∼5-7 keV band during the period of outburst
  that could be interpreted as a relativistic Fe Kα emission line. Our
  analysis suggests that its flux has increased in tandem with the 2-10
  keV continuum, making it the second changing look AGN in which the broad
  Fe Kα line responds to the X-ray continuum variability. This behavior
  strongly supports the idea that X-rays originates in a corona above
  the accretion disk, and disk reflection produces the relativistic Fe
  Kα line. In addition, we find the response of narrow Fe Kα emission
  line to the changes in the X-ray continuum on a time-scale as short
  as four months, allowing to put the location of line-emitting region
  at &lt;0.1 pc, comparable to the size of optical BLR. By comparing to
  the changing look AGN NGC 2992, the Fe Kα variation rate (the ratio
  of Fe Kα variation to luminosity variation) in NGC 1566 appears
  greater, which could be possibly explained by larger amount of gas
  or Fe abundance responsible for producing the Fe Kα line for the
  latter. The strength of variable broad Fe Kα line as well as the soft
  X-ray excess emission appears to be correlated with the accretion rate,
  which could be explained as due to the state transition associated
  with the changing-look phenomenon.

Title: A Dynamo-Based Prediction of Solar Cycle 25
Authors: Guo, Wei; Jiang, Jie; Wang, Jing-Xiu
Bibcode: 2021SoPh..296..136G
Altcode: 2021arXiv210801412G
  The solar activity cycle varies in amplitude. The last Solar Cycle 24 is
  the weakest in the past century. Sun's activity dominates Earth's space
  environment. The frequency and intensity of Sun's activity follow the
  solar cycle. Hence there are practical needs to know the amplitude of
  the upcoming Solar Cycle 25. Dynamo-based solar cycle predictions not
  only provide forecasts, but also offer an effective way to evaluate our
  understanding of the solar cycle. In this article we apply the method
  of the first successful dynamo-based prediction developed for Solar
  Cycle 24 to predict Solar Cycle 25, so that we can verify whether the
  previous success is repeatable. The prediction shows that Solar Cycle
  25 would be about 10% stronger than Solar Cycle 24 with an amplitude
  of 126 (international sunspot number Version 2.0). The result suggests
  that Solar Cycle 25 will not be the beginning of a Maunder-like grand
  solar minimum as suggested by some publications. The solar behavior in
  about four to five years will confirm whether the prediction method
  captures the key mechanism for solar cycle variability, which is the
  polar field around the cycle minimum in our model.

Title: Algebraic quantification of an active region contribution to
    the solar cycle
Authors: Wang, Zi-Fan; Jiang, Jie; Wang, Jing-Xiu
Bibcode: 2021A&A...650A..87W
Altcode: 2021arXiv210404307W
  Context. The solar dipole moment at cycle minimum is considered to be
  the most reliable precursor with which to determine the amplitude of the
  subsequent cycle. Numerical simulations of the surface flux transport
  (SFT) model are widely used to effectively predict the dipole moment
  at cycle minimum. An algebraic method was recently proposed to quickly
  predict the contribution of an active region (AR) to the axial dipole
  moment at cycle minimum instead of SFT simulations. The method assumes
  a bipolar magnetic region (BMR) configuration of ARs, however most ARs
  are asymmetric in configuration of opposite polarities, or have more
  complex configurations. Such ARs evolve significantly differently from
  those of BMR approximations. <BR /> Aims: We propose a generalized
  algebraic method to describe the axial dipole contribution of an
  AR with an arbitrary configuration, and evaluate its effectiveness
  compared to the BMR-based method. <BR /> Methods: We employ mathematical
  deductions to obtain the generalized method. We compare the results
  of the generalized method with SFT simulations of observed ARs,
  artificially created BMRs, and ARs with more complex configurations. We
  also compare the results with those from the BMR-based method. <BR
  /> Results: The generalized method is equivalent to the SFT model,
  and precisely predicts the contributions of ARs to the dipole moment,
  but has a much higher computational efficiency. Although the BMR-based
  method has similar computational efficiency to the generalized method,
  it is only accurate for symmetric bipolar ARs. The BMR-based method
  systematically overestimates the dipole contributions of asymmetric
  bipolar ARs, and randomly miscalculates the contributions of more
  complex ARs. <BR /> Conclusions: The generalized method provides a
  quick and precise quantification of the contribution of an AR to solar
  cycle evolution, which paves the way for application in physics-based
  solar cycle predictions.

Title: Homologous Microflares with Mass Ejection and Plasma Heating
    on the Quiet Sun
Authors: Jin, C. L.; Zhou, G. P.; Wang, J. X.
Bibcode: 2021ApJ...914L..35J
Altcode:
  Study of microflares on the quiet Sun is extremely important in learning
  the physics of both solar flare and atmospheric heating. Here, for the
  first time, we report the detailed observations of two homologous
  microflares from Atmospheric Imager Assembly (AIA) images and
  Heliospheric Magnetic Imager magnetograms in a very quiet region. The
  two microflares are observed clearly in the extreme ultraviolet and
  faintly in the ultraviolet in AIA images. They have an area of 59
  Mm<SUP>2</SUP> and 46 Mm<SUP>2</SUP>, and a duration of 25 minutes
  and 22 minutes. The magnetic cancellation continuously takes place
  during the microflares, and the magnetic flux decrease is apparent,
  with a value of 4 10<SUP>18</SUP> Mx. The obvious mass ejections
  are observed during the microflares, and dimming occurs during and
  after the microflares. The velocity of mass ejection is up to 160 km
  s<SUP>1</SUP>. For the two microflares, the time of peak intensity
  in 30.4 nm precedes that of the coronal peak emission, up to 2.43.3
  minutes. Their thermal energy is estimated to be 1.3 10<SUP>27</SUP>
  erg and 2.5 10<SUP>26</SUP> erg, respectively, which heats the corona
  up to 5.8 MK and 2.8 MK. There are many similarities of microflares
  on the quiet Sun to major flares in the active regions.

Title: Physical Parameters of the Eclipsing Binary System EPIC
    202060577
Authors: Zhao, S. J.; Fu, J. N.; Wang, J. T.; Li, C. Q.; Wang, J. X.;
   Zong, W. K.
Bibcode: 2021AcASn..62...23Z
Altcode:
  EPIC 202060577 is an eclipsing binary system containing a B-type
  primary star. From the K2 photometry, 45 secondary minimal times were
  obtained. The orbital period is determined to be 1.019648 days and the
  epoch formula is derived. Based on LAMOST (Large Sky Area Multi-Object
  Fiber Spectroscopic Telescope) spectra, the ROTFIT program is used
  to obtain spectral class, effective temperature, metal abundance
  and surface gravity of the primary star, and calculate the radial
  velocities. Through the PHOEBE (Physics Of Eclipsing Binaries)
  modeling program and emcee (Affine Invariant Markov chain Monte
  Carlo Ensemble Sampler) fitting program, a solution of the orbital
  parameters is obtained and the influence of Rossiter-McLaughlin effect
  on the radial velocity curve is analyzed. The final solution shows
  that EPIC 202060577 is a detached eclipsing binary system with mass
  ratio q=0.11, the spectral class of the primary star is B2/3. The
  mass, radius and effective temperature of the primary and secondary
  stars are M_1=12.56M_{⊙} and M_2= 1.39M_{⊙}, R_1=4.58R_{sun} and
  R_2=1.85R_{rm sun}, T_1=18979 K and T_2=8710 K, respectively, here
  M_{⊙} and R_{sun} are the solar mass and solar radius. According
  to the physical parameters, the evolutionary phase of EPIC 202060577
  is discussed.

Title: Activity Complexes and a Prominent Poleward Surge during
    Solar Cycle 24
Authors: Wang, Zi-Fan; Jiang, Jie; Zhang, Jie; Wang, Jing-Xiu
Bibcode: 2020ApJ...904...62W
Altcode: 2020arXiv200912483W
  Long-lasting activity complexes (ACs), characterized as a series of
  closely located, continuously emerging solar active regions (ARs), are
  considered generating prominent poleward surges from observations. The
  surges lead to significant variations of the polar field, which
  are important for the modulation of solar cycles. We aim to study
  a prominent poleward surge during solar cycle 24 on the southern
  hemisphere, and analyze its originating ACs and the effect on the
  polar field evolution. We automatically identify and characterize ARs
  based on synoptic magnetograms from the Solar Dynamics Observatory. We
  assimilate these ARs with realistic magnetic configuration into a
  surface flux transport model, and simulate the creation and migration
  of the surge. Our simulations well reproduce the characteristics
  of the surge and show that the prominent surge is mainly caused by
  the ARs belonging to two ACs during Carrington rotations 2145-2159
  (2013 December-2015 January). The surge has a strong influence on the
  polar field evolution of the southern hemisphere during the latter
  half of cycle 24. Without the about one-year-long flux emergence in
  the form of ACs, the polar field around the cycle minimum would have
  remained at a low level and even reversed to the polarity at cycle 23
  minimum. Our study also shows that the long-lived unipolar regions due
  to the decay of the earlier emerging ARs cause an intrinsic difficulty
  of automatically identifying and precisely quantifying later emerging
  ARs in ACs.

Title: VizieR Online Data Catalog: Sun active regions from 1976-2017
    (Jiang+, 2019)
Authors: Jiang, J.; Song, Q.; Wang, J. -X.; Baranyi, T.
Bibcode: 2020yCat..18710016J
Altcode:
  The Debrecen Photoheliographic Data (DPD) sunspot catalog (Baranyi+,
  2016SoPh..291.3081B) is the most detailed and user-friendly catalog
  at present. It provides the area and position data for each observable
  sunspot and sunspot groups on a daily basis along with images of sunspot
  groups, full-disk scans, and magnetograms starting from 1974 to the
  present. <P />The Geostationnary Operational Environmental Satellites
  (GOES) X-ray data are available from 1975 September onwards. We select
  ARs that are larger than 800{micro}Hem from the beginning of 1976 to
  the end of 2017. The 567 ARs that satisfy this requirement are singled
  out as our samples. <P />(1 data file).

Title: Accurate focusing technology for the coronal images
Authors: Zhang, X. F.; Liu, Y.; Li, X. B.; Song, T. F.; Zhao, M. Y.;
   Wang, J. X.
Bibcode: 2019SPIE11116E..1DZ
Altcode:
  Optical imaging has been widely used in many fields as a tool for
  acquiring images, which can be used in microscopic observation,
  medical analysis, remote sensing, and astronomical observation. In
  the field of astronomical observations, it is very important to adjust
  the focus of the coronagraph. Due to the significant differences of the
  intensity between the corona and the solar photosphere, the ground-based
  coronagraph usually adopt an occulter, which is a little larger than
  the solar disk, to shield the light from the solar photosphere. In
  absence of the Sun as reference, focusing of the coronagraph is much
  harder than usual optical system. For the ground-based coronagraph,
  we developed a method of focusing using the solar disk image behind
  this disk occulter. Based on a series of images collected by shifting
  the center of the solar disk, we extract edge information of the solar
  disk and use the edge gradient algorithm to fit the focal length. This
  method can reduce the error of manual focusing. We can precisely find
  out the coronagraph focal point and obtain a clear coronal image,
  which lays a foundation for the technical support about remote control
  system of the coronagraph.

Title: Magnetic flux participation in solar surface magnetism during
    solar cycle 24
Authors: Jin, Chun-Lan; Wang, Jing-Xiu
Bibcode: 2019RAA....19...69J
Altcode:
  This study aims at investigating surface magnetic flux participation
  among different types of magnetic features during solar cycle
  24. State-of-the-art observations from SDO/HMI and Hinode/SOT are
  combined to form a unique database in the interval from April 2010
  to October 2015. Unlike previous studies, the statistics presented in
  this paper are feature-detection-based. More than 20 million magnetic
  features with relatively large scale, such as sunspot/pore, enhanced
  and quiet networks, are automatically detected and categorized from
  HMI observations, and the internetwork features are identified from
  SOT/SP observations. The total flux from these magnetic features reaches
  5.9×10<SUP>22</SUP> Mx during solar minimum and 2.4×10<SUP>23</SUP>
  Mx in solar maximum. Flux occupation from the sunspot/pore region is
  29% in solar maximum. Enhanced and quiet networks contribute 18% and
  21% flux during the solar minimum, and 50% and 9% flux in the solar
  maximum respectively. The internetwork field contributes over 55%
  of flux in the solar minimum, and its flux contribution exceeds that
  of sunspot/pore features in the solar maximum. During the solar active
  condition, the sunspot field increases its area but keeps constant flux
  density of about 150G, while the enhanced network follows the sunspot
  number variation showing increasing flux density and area, but the quiet
  network displays decreasing area and somewhat increasing flux density
  of about 6%. The origin of the quiet network is not known exactly,
  but is suggestive of representing the interplay between mean-field
  and local dynamos. The source, magnitude and possible importance of
  ‘hidden flux’ are discussed in some detail.

Title: A magnetar-powered X-ray transient as the aftermath of a
    binary neutron-star merger
Authors: Xue, Y. Q.; Zheng, X. C.; Li, Y.; Brandt, W. N.; Zhang,
   B.; Luo, B.; Zhang, B. -B.; Bauer, F. E.; Sun, H.; Lehmer, B. D.;
   Wu, X. -F.; Yang, G.; Kong, X.; Li, J. Y.; Sun, M. Y.; Wang, J. -X.;
   Vito, F.
Bibcode: 2019Natur.568..198X
Altcode: 2019arXiv190405368X
  Mergers of neutron stars are known to be associated with short
  γ-ray bursts<SUP>1-4</SUP>. If the neutron-star equation of state is
  sufficiently stiff (that is, the pressure increases sharply as the
  density increases), at least some such mergers will leave behind a
  supramassive or even a stable neutron star that spins rapidly with
  a strong magnetic field<SUP>5-8</SUP> (that is, a magnetar). Such
  a magnetar signature may have been observed in the form of the
  X-ray plateau that follows up to half of observed short γ-ray
  bursts<SUP>9,10</SUP>. However, it has been expected that some X-ray
  transients powered by binary neutron-star mergers may not be associated
  with a short γ-ray burst<SUP>11,12</SUP>. A fast X-ray transient (CDF-S
  XT1) was recently found to be associated with a faint host galaxy, the
  redshift of which is unknown<SUP>13</SUP>. Its X-ray and host-galaxy
  properties allow several possible explanations including a short γ-ray
  burst seen off-axis, a low-luminosity γ-ray burst at high redshift, or
  a tidal disruption event involving an intermediate-mass black hole and
  a white dwarf<SUP>13</SUP>. Here we report a second X-ray transient,
  CDF-S XT2, that is associated with a galaxy at redshift z = 0.738
  (ref. <SUP>14</SUP>). The measured light curve is fully consistent
  with the X-ray transient being powered by a millisecond magnetar. More
  intriguingly, CDF-S XT2 lies in the outskirts of its star-forming host
  galaxy with a moderate offset from the galaxy centre, as short γ-ray
  bursts often do<SUP>15,16</SUP>. The estimated event-rate density
  of similar X-ray transients, when corrected to the local value, is
  consistent with the event-rate density of binary neutron-star mergers
  that is robustly inferred from the detection of the gravitational-wave
  event GW170817.

Title: Multiple Magnetic Reconnections Driven by a Large-scale
    Magnetic Flux Rope
Authors: Zhou, G. P.; Tan, C. M.; Su, Y. N.; Shen, C. L.; Tan, B. L.;
   Jin, C. L.; Wang, J. X.
Bibcode: 2019ApJ...873...23Z
Altcode:
  Magnetic flux ropes (MFRs), as the most probable core structure
  of solar eruptive activity, remain mysterious on their origination,
  magnetic environment, and erupting mechanisms. Here, we newly identify
  a large-scale hot channel MFR, named “MFR3”, that connects an
  anti-Hale active region (AR) 11429 and a normal AR 11430 on 2012
  March 7 based on multi-wavelength observations. An oscillation is
  first detected at the top of MFR3 during 00:10-00:30 UT as triggered
  by an X5.4 flare-related eruption of an MFR (named “MFR1” here)
  in AR 11429. Then, after a quiet period of ∼20 minutes at around
  00:52 UT, external magnetic reconnection (EMR) occurred above MFR3
  manifested by not only bidirectional outflow in extreme ultraviolet
  images, but also microwave quasi-periodic pulsation in broadband radio
  spectral observations for the first time. With the occurrence of EMR,
  the large-scale MFR3 quickly erupted at 01:01 UT and triggered an
  X1.3 flare, which is related to the eruption of the other MFR (named
  “MFR2” here) in AR 11429 at 01:05 UT. The erupting MFR3 and MFR2
  appeared successively in the same associated halo coronal mass ejection
  (CME) as two different core structures. The identification of the
  large-scale MFR3 between two separated ARs and its complex activity
  may shed new light on our understanding of the initiation mechanism
  of a CME. Further work should lay emphasis on how a large-scale MFR3
  forms in the solar atmosphere.

Title: Different Contributions to Space Weather and Space Climate
    from Different Big Solar Active Regions
Authors: Jiang, Jie; Song, Qiao; Wang, Jing-Xiu; Baranyi, Tünde
Bibcode: 2019ApJ...871...16J
Altcode: 2019arXiv190100116J
  The purpose of this paper is to show that large active regions (ARs)
  with different magnetic configurations have different contributions
  to short-term and long-term variations of the Sun. As a case study,
  the complex δ-type AR 12673 and the simple β-type AR 12674 are
  investigated in detail. Since the axial dipole moment at cycle minimum
  determines the amplitude of the subsequent cycle and space climate,
  we have assimilated the individual observed magnetic configurations
  of these two ARs into a surface flux transport model to compare their
  contributions to the axial dipole moment D. We find that AR 12673 has
  a significant effect on D at the end of the cycle, making it weaker
  because of abnormal and complicated magnetic polarities. An initial
  strongly positive D ends up with a strongly negative value. The
  flare-poor AR 12674 has a greater contribution to the long-term
  axial dipole moment than the flare-rich AR 12673. We then carry out a
  statistical analysis of ARs larger than 800 μHem from 1976 to 2017. We
  use the flare index FI and define an axial dipole moment index DI to
  quantify the effects of each AR on space weather and space climate,
  respectively. Whereas the FI has a strong dependence on the magnetic
  configuration, the DI shows no such dependence. The DI is mainly
  determined by the latitudinal location and the latitudinal separation
  of the positive and negative magnetic fluxes of the ARs. Simple ARs
  have the same possibility as complex ARs to produce big DI values
  affecting space climate.

Title: Variability-selected Low-luminosity Active Galactic Nuclei
    Candidates in the 7 Ms Chandra Deep Field-South
Authors: Ding, N.; Luo, B.; Brandt, W. N.; Paolillo, M.; Yang, G.;
   Lehmer, B. D.; Shemmer, O.; Schneider, D. P.; Tozzi, P.; Xue, Y. Q.;
   Zheng, X. C.; Gu, Q. S.; Koekemoer, A. M.; Vignali, C.; Vito, F.;
   Wang, J. X.
Bibcode: 2018ApJ...868...88D
Altcode: 2018arXiv181009465D
  In deep X-ray surveys, active galactic nuclei (AGNs) with a broad range
  of luminosities have been identified. However, cosmologically distant
  low-luminosity AGN (LLAGN, {L}<SUB>{{X</SUB>}}≲ {10}<SUP>42</SUP>
  erg s<SUP>-1</SUP>) identification still poses a challenge because
  of significant contamination from host galaxies. Based on the 7 Ms
  Chandra Deep Field-South (CDF-S) survey, the longest-timescale (∼17
  years) deep X-ray survey to date, we utilize an X-ray variability
  selection technique to search for LLAGNs that remain unidentified
  among the CDF-S X-ray sources. We find 13 variable sources from 110
  unclassified CDF-S X-ray sources. Except for one source that could
  be an ultraluminous X-ray source, the variability of the remaining 12
  sources is most likely due to accreting supermassive black holes. These
  12 AGN candidates have low intrinsic X-ray luminosities, with a
  median value of 7 × 10<SUP>40</SUP> erg s<SUP>-1</SUP>. They are
  generally not heavily obscured, with an average effective power-law
  photon index of 1.8. The fraction of variable AGNs in the CDF-S is
  independent of X-ray luminosity and is only restricted by the total
  number of observed net counts, confirming previous findings that X-ray
  variability is a near-ubiquitous property of AGNs over a wide range of
  luminosities. There is an anticorrelation between X-ray luminosity and
  variability amplitude for high-luminosity AGNs, but as the luminosity
  drops to ≲10<SUP>42</SUP> erg s<SUP>-1</SUP>, the variability
  amplitude no longer appears dependent on the luminosity. The entire
  observed luminosity-variability trend can be roughly reproduced by
  an empirical AGN variability model based on a broken power-law power
  spectral density function.

Title: A unique distant submillimeter galaxy with an X-ray-obscured
    radio-luminous active galactic nucleus
Authors: Shu, X. W.; Xue, Y. Q.; Liu, D. Z.; Wang, T.; Han, Y. K.;
   Chang, Y. Y.; Liu, T.; Huang, X. X.; Wang, J. X.; Zheng, X. Z.;
   da Cunha, E.; Daddi, E.; Elbaz, D.
Bibcode: 2018A&A...619A..76S
Altcode: 2018arXiv180900318S
  <BR /> Aims: We present a multiwavelength study of an atypical
  submillimeter galaxy, GH500.30, in the GOODS-North field, with the aim
  to understand its physical properties of stellar and dust emission, as
  well as the central active galactic nucleus (AGN) activity. Although
  it is shown that the source is likely an extremely dusty galaxy
  at high redshift, its exact position of submillimeter emission is
  unknown. <BR /> Methods: We use NOEMA observation at 1.2 mm with
  subarcsecond resolution to resolve the dust emission, and precisely
  localize the counterparts at other wavelengths, which allows us to
  better constrain its stellar and dust spectral energy distribution
  (SED) as well as redshift. We carry out the new near-infrared (NIR)
  photometry of GH500.30 observed with HST, and perform panchromatic SED
  modelling from ultraviolet (UV)/optical to submillimeter. We derive the
  photometric redshift using both NIR and far-infrared (FIR) SED modeling,
  and place constraints on the stellar and dust properties such as stellar
  mass, age, dust attenuation, IR luminosity, and star-formation rate
  (SFR). The AGN properties are inferred from the X-ray spectral analysis
  and radio observations, and its contribution to the total IR luminosity
  is estimated from the broadband SED fittings using MAGPHYS. <BR />
  Results: With the new NOEMA interferometric imaging, we confirm that
  the source is a unique dusty galaxy. It has no obvious counterpart
  in the optical and even NIR images observed with HST at λ ≲ 1.4
  μm. Photometric-redshift analyses from both stellar and dust SED
  suggest it to likely be at z ≳ 4, though a lower redshift at z ≳ 3.1
  cannot be fully ruled out (at 90% confidence interval). Explaining its
  unusual optical-to-NIR properties requires an old stellar population
  (∼0.67 Gyr), coexisting with a very dusty ongoing starburst
  component. The latter is contributing to the FIR emission, with its
  rest-frame UV and optical light being largely obscured along our
  line of sight. If the observed fluxes at the rest-frame optical/NIR
  wavelengths were mainly contributed by old stars, a total stellar mass
  of ∼3.5 × 10<SUP>11</SUP> M<SUB>⊙</SUB> would be obtained. An
  X-ray spectral analysis suggests that this galaxy harbors a heavily
  obscured AGN with N<SUB>H</SUB> = 3.3<SUP>+2.0</SUP><SUB>-1.7</SUB>
  × 10<SUP>23</SUP> cm<SUP>-2</SUP> and an intrinsic 2-10 keV luminosity
  of L<SUB>x</SUB> ∼ 2.6 × 10<SUP>44</SUP> erg s<SUP>-1</SUP>, which
  places this object among distant type 2 quasars. The radio emission of
  the source is extremely bright, which is an order of magnitude higher
  than the star-formation-powered emission, making it one of the most
  distant radio-luminous dusty galaxies. <BR /> Conclusions: The combined
  characteristics of the galaxy suggest that the source appears to have
  been caught in a rare but critical transition stage in the evolution
  of submillimeter galaxies, where we are witnessing the birth of a young
  AGN and possibly the earliest stage of its jet formation and feedback.

Title: Predictability of the Solar Cycle Over One Cycle
Authors: Jiang, Jie; Wang, Jing-Xiu; Jiao, Qi-Rong; Cao, Jin-Bin
Bibcode: 2018ApJ...863..159J
Altcode: 2018arXiv180701543J
  The prediction of the strength of future solar cycles is of interest
  because of its practical significance for space weather and as a test of
  our theoretical understanding of the solar cycle. The Babcock-Leighton
  mechanism allows predictions by assimilating the observed magnetic
  field on the surface. Since the emergence of sunspot groups has
  random properties, making it impossible to accurately predict the
  solar cycle and strongly limiting the scope of cycle predictions,
  we develop a scheme to investigate the predictability of the solar
  cycle over one cycle. When a cycle has been ongoing for more than
  three years, the sunspot group emergence can be predicted along with
  its uncertainty during the rest time of the cycle. The method for
  this prediction is to start by generating a set of random realizations
  that obey the statistical relations of the sunspot emergence. We then
  use a surface flux transport model to calculate the possible axial
  dipole moment evolutions. The correlation between the axial dipole
  moment at cycle minimum and the subsequent cycle strength and other
  empirical properties of solar cycles are used to predict the possible
  profiles of the subsequent cycle. We apply this scheme to predict the
  large-scale field evolution from 2018 to the end of cycle 25, whose
  maximum strength is expected to lie in the range from 93 to 155 with
  a probability of 95%.

Title: A Long Decay of X-Ray Flux and Spectral Evolution in the
    Supersoft Active Galactic Nucleus GSN 069
Authors: Shu, X. W.; Wang, S. S.; Dou, L. M.; Jiang, N.; Wang, J. X.;
   Wang, T. G.
Bibcode: 2018ApJ...857L..16S
Altcode: 2018arXiv180900319S
  GSN 069 is an optically identified very low-mass active galactic
  nuclei (AGN) that shows supersoft X-ray emission. The source is known
  to exhibit a huge X-ray outburst, with flux increased by more than
  a factor of ∼240 compared to the quiescence state. We report its
  long-term evolution in the X-ray flux and spectral variations over a
  timescale of ∼decade, using both new and archival X-ray observations
  from the XMM-Newton and Swift. The new Swift observations detected
  the source in its lowest level of X-ray activity since the outburst,
  a factor of ∼4 lower in the 0.2-2 keV flux than that obtained with
  the XMM-Newton observations nearly eight years ago. Combining with the
  historical X-ray measurements, we find that the X-ray flux is decreasing
  slowly. There seemed to be spectral softening associated with the
  drop of X-ray flux. In addition, we find evidence for the presence of
  a weak, variable, hard X-ray component, in addition to the dominant
  thermal blackbody emission reported before. The long decay of X-ray
  flux and spectral evolution, as well as the supersoft X-ray spectra,
  suggest that the source could be a tidal disruption event (TDE), though
  a highly variable AGN cannot be fully ruled out. Further continued
  X-ray monitoring would be required to test the TDE interpretation,
  by better determining the flux evolution in the decay phase.

Title: Linking black hole growth with host galaxies: the
    accretion-stellar mass relation and its cosmic evolution
Authors: Yang, G.; Brandt, W. N.; Vito, F.; Chen, C. -T. J.; Trump,
   J. R.; Luo, B.; Sun, M. Y.; Xue, Y. Q.; Koekemoer, A. M.; Schneider,
   D. P.; Vignali, C.; Wang, J. -X.
Bibcode: 2018MNRAS.475.1887Y
Altcode: 2017arXiv171009399Y
  Previous studies suggest that the growth of supermassive black holes
  (SMBHs) may be fundamentally related to host-galaxy stellar mass
  (M<SUB>⋆</SUB>). To investigate this SMBH growth-M<SUB>⋆</SUB>
  relation in detail, we calculate long-term SMBH accretion rate as a
  function of M<SUB>⋆</SUB> and redshift [\overlineBHAR(M_{\star },
  z)] over ranges of log (M<SUB>⋆</SUB>/M<SUB>⊙</SUB>) = 9.5-12
  and z = 0.4-4. Our \overlineBHAR(M_{\star }, z) is constrained by
  high-quality survey data (GOODS-South, GOODS-North and COSMOS), and
  by the stellar mass function and the X-ray luminosity function. At a
  given M<SUB>⋆</SUB>, \overlineBHAR is higher at high redshift. This
  redshift dependence is stronger in more massive systems [for log
  (M<SUB>⋆</SUB>/M<SUB>⊙</SUB>) ≈ 11.5, \overlineBHAR is three
  decades higher at z = 4 than at z = 0.5], possibly due to AGN
  feedback. Our results indicate that the ratio between \overlineBHAR
  and average star formation rate (\overlineSFR) rises towards high
  M<SUB>⋆</SUB> at a given redshift. This \overlineBHAR/\overlineSFR
  dependence on M<SUB>⋆</SUB> does not support the scenario that
  SMBH and galaxy growth are in lockstep. We calculate SMBH mass
  history [M<SUB>BH</SUB>(z)] based on our \overlineBHAR(M_{\star },
  z) and the M<SUB>⋆</SUB>(z) from the literature, and find that the
  M<SUB>BH</SUB>-M<SUB>⋆</SUB> relation has weak redshift evolution
  since z ≈ 2. The M<SUB>BH</SUB>/M<SUB>⋆</SUB> ratio is higher
  towards massive galaxies: it rises from ≈1/5000 at log M<SUB>⋆</SUB>
  ≲ 10.5 to ≈1/500 at log M<SUB>⋆</SUB> ≳ 11.2. Our predicted
  M<SUB>BH</SUB>/M<SUB>⋆</SUB> ratio at high M<SUB>⋆</SUB> is similar
  to that observed in local giant ellipticals, suggesting that SMBH
  growth from mergers is unlikely to dominate over growth from accretion.

Title: Automatic Solar Seeing Observations at Mt. Wumingshan in
    Western China
Authors: Song, T. F.; Wen, Y. M.; Liu, Y.; Elmhamdi, A.; Kordi,
   A. S.; Zhao, M. Y.; Zhang, X. F.; Li, X. B.; Wang, J. X.; Fu, Y.;
   Cheng, X. M.; Xu, F. Y.
Bibcode: 2018SoPh..293...37S
Altcode:
  Mountain Wumingshan (Mt. WMS) is located in the southeastern foot
  of the Tibet Plateau with an altitude of 4,800 m. It is one of the
  candidate sites to place China's next-generation large-scale solar
  telescope. A temporary observation platform has been built at Mt. WMS,
  but there is still a great need of a stable solar-seeing monitoring for
  long-term observations. Based on the preliminary studies on the Solar
  Differential Image Motion Monitor (SDIMM) of the Yunnan Observatories,
  we built an improved version of this early prototype, which is
  called Wumingshan Mountain Automated Solar Differential Image Motion
  Monitor (WMA-SDIMM). We develop the automatic system of the WMA-SDIMM,
  investigate the reliability and precision of our measurements by error
  analysis and comparison testing, and present the statistical results
  from October 2016 to September 2017 at Mt. WMS. WMA-SDIMM works very
  well at Mt. WMS and is quite suitable for long-period daytime seeing
  observations.

Title: A prediction of the solar cycle 25
Authors: Jiang, Jie; Wang, Jing-Xiu; Jiao, Qi-Rong
Bibcode: 2018IAUS..340..327J
Altcode:
  Here we report our recent prediction of the solar cycle 25 based on a
  newly developed scheme, which is used to investigate the predictability
  of the solar cycle over one cycle. The scheme is a combination of the
  empirical properties of solar cycles and a surface flux transport model
  to get the possible axial dipole moment evolution at a few years before
  cycle minimum, by which to get the subsequent cycle strength based on
  the correlation between the axial dipole moment at cycle minimum and
  the subsequent cycle strength. We apply this scheme to predict the
  large-scale field evolution since 2018 onwards. The results show that
  the northern polar field will keep on increasing, while the southern
  polar field almost keeps flat by the end of cycle 24. This leads to
  the cycle 25 strength of 125 +/- 32, which is about 10% stronger than
  cycle 24 according to the mean value.

Title: A Study of External Magnetic Reconnection that Triggers a
    Solar Eruption
Authors: Zhou, G. P.; Zhang, J.; Wang, J. X.; Wheatland, M. S.
Bibcode: 2017ApJ...851L...1Z
Altcode:
  External magnetic reconnection (EMR) is suggested to play an
  essential role in triggering a solar eruption, but is rarely directly
  observed. Here, we report on a filament eruption on 2014 October 3
  that apparently involves the process of an early EMR. A total of 1.7 ×
  10<SUP>20</SUP> Mx flux was first canceled along the filament-related
  polarity inversion line over 12 hr, and then the filament axis started
  to brighten in extreme ultraviolet (EUV). An impulsive EUV brightening
  began 30 minutes later, and we attribute this to EMR, as it is located
  at the center of a bidirectional outflow with a velocity of 60-75 km
  s<SUP>-1</SUP> along large-scale magnetic loops from active regions
  NOAA 12178 and 12179, respectively, and over the filament mentioned
  above. Following the EMR, the filament was activated; then, partial
  eruption occurred 6 minutes later in the west, in which the decay
  index above the magnetic flux rope (MFR) reached the critical value of
  1.5. The observations are interpreted in terms of underlying magnetic
  flux cancelation leading to the buildup and eventual formation of the
  MFR with a filament embedded in it, and the MFR is elevated later. The
  activated MFR rises and pushes the overlying sheared field and forms a
  current sheet causing the EMR. The EMR in turn weakens the constraining
  effect of the overlying field, leading to the arising of the MFR,
  and subsequently erupting due to torus instability.

Title: Deepest View of AGN X-Ray Variability with the 7 Ms Chandra
    Deep Field-South Survey
Authors: Zheng, X. C.; Xue, Y. Q.; Brandt, W. N.; Li, J. Y.; Paolillo,
   M.; Yang, G.; Zhu, S. F.; Luo, B.; Sun, M. Y.; Hughes, T. M.; Bauer,
   F. E.; Vito, F.; Wang, J. X.; Liu, T.; Vignali, C.; Shu, X. W.
Bibcode: 2017ApJ...849..127Z
Altcode: 2017arXiv171004358Z
  We systematically analyze the X-ray variability of active galactic
  nuclei (AGNs) in the 7 Ms Chandra Deep Field-South survey. On the
  longest timescale (≈17 years), we find only a weak (if any)
  dependence of X-ray variability amplitudes on energy bands or
  obscuration. We use four different power spectral density (PSD)
  models to fit the anticorrelation between normalized excess variance
  ({σ }<SUB>{nxv</SUB>}<SUP>2</SUP>) and luminosity, and obtain a
  best-fit power-law index β ={1.16}<SUB>-0.05</SUB><SUP>+0.05</SUP>
  for the low-frequency part of the AGN PSD. We also divide the whole
  light curves into four epochs in order to inspect the dependence
  of {σ }<SUB>{nxv</SUB>}<SUP>2</SUP> on these timescales, finding
  an overall increasing trend. The analysis of these shorter
  light curves also infers a β of ∼1.3 that is consistent
  with the above-derived β, which is larger than the frequently
  assumed value of β =1. We then investigate the evolution of {σ
  }<SUB>{nxv</SUB>}<SUP>2</SUP>. No definitive conclusion is reached
  because of limited source statistics, but if present, the observed
  trend goes in the direction of decreasing AGN variability at fixed
  luminosity toward high redshifts. We also search for transient events
  and find six notable candidate events with our considered criteria. Two
  of them may be a new type of fast transient events, one of which is
  reported here for the first time. We therefore estimate a rate of fast
  outbursts &lt; \dot{N}&gt; ={1.0}<SUB>-0.7</SUB><SUP>+1.1</SUP>×
  {10}<SUP>-3</SUP> {{galaxy}}<SUP>-1</SUP> {{yr}}<SUP>-1</SUP> and a
  tidal disruption event (TDE) rate &lt; {\dot{N}}<SUB>{TDE</SUB>}&gt;
  ={8.6}<SUB>-4.9</SUB><SUP>+8.5</SUP>× {10}<SUP>-5</SUP>
  {{galaxy}}<SUP>-1</SUP> {{yr}}<SUP>-1</SUP> assuming the other four
  long outbursts to be TDEs.

Title: Tracing the accretion history of supermassive black holes
through X-ray variability: results from the ChandraDeep Field-South
Authors: Paolillo, M.; Papadakis, I.; Brandt, W. N.; Luo, B.; Xue,
   Y. Q.; Tozzi, P.; Shemmer, O.; Allevato, V.; Bauer, F. E.; Comastri,
   A.; Gilli, R.; Koekemoer, A. M.; Liu, T.; Vignali, C.; Vito, F.;
   Yang, G.; Wang, J. X.; Zheng, X. C.
Bibcode: 2017MNRAS.471.4398P
Altcode: 2017arXiv170705332P
  We study the X-ray variability properties of distant active galactic
  nuclei (AGNs) in the ChandraDeep Field-South region over 17 yr, up
  to z ∼ 4, and compare them with those predicted by models based
  on local samples. We use the results of Monte Carlo simulations to
  account for the biases introduced by the discontinuous sampling and
  the low-count regime. We confirm that variability is a ubiquitous
  property of AGNs, with no clear dependence on the density of the
  environment. The variability properties of high-z AGNs, over different
  temporal time-scales, are most consistent with a power spectral density
  (PSD) described by a broken (or bending) power law, similar to nearby
  AGNs. We confirm the presence of an anticorrelation between luminosity
  and variability, resulting from the dependence of variability on black
  hole (BH) mass and accretion rate. We explore different models, finding
  that our acceptable solutions predict that BH mass influences the value
  of the PSD break frequency, while the Eddington ratio λ<SUB>Edd</SUB>
  affects the PSD break frequency and, possibly, the PSD amplitude as
  well. We derive the evolution of the average λ<SUB>Edd</SUB> as a
  function of redshift, finding results in agreement with measurements
  based on different estimators. The large statistical uncertainties make
  our results consistent with a constant Eddington ratio, although one of
  our models suggest a possible increase of λ<SUB>Edd</SUB> with lookback
  time up to z ∼ 2-3. We conclude that variability is a viable mean to
  trace the accretion history of supermassive BHs, whose usefulness will
  increase with future, wide-field/large effective area X-ray missions.

Title: VizieR Online Data Catalog: 16yrs of AGNs X-ray spectral
    analyses from 7Ms CDF-S (Liu+, 2017)
Authors: Liu, T.; Tozzi, P.; Wang, J. -X.; Brandt, W. N.; Vignali,
   C.; Xue, Y.; Schneider, D. P.; Comastri, A.; Yang, G.; Bauer, F. E.;
   Paolillo, M.; Luo, B.; Gilli, R.; Wang, Q. D.; Giavalisco, M.; Ji,
   Z.; Alexander, D. M.; Mainieri, V.; Shemmer, O.; Koekemoer, A.;
   Risaliti, G.
Bibcode: 2017yCat..22320008L
Altcode:
  The 7Ms CDF-S survey is comprised of observations performed between
  1999 October 14, and 2016 March 24, (UTC). Excluding one observation
  compromised by telemetry saturation and other issues (ObsID 581),
  there are 102 observations (observation IDs listed in Table 1) in
  the data set. The exposures collected across 16 years can be grouped
  into four distinct periods, each spanning 2-21 months. <P />Table 1:
  ---------------------------------------------------------------------------
  Period Observation Date Time Span Exposure Time
  ---------------------------------------------------------------------------
  I 1999.10-2000.12 14 months 1Ms 11 ObsIDs: 1431-0 1431-1 441 582 2406
  2405 2312 1672 2409 2313 2239 <P />II 2007.09-2007.11 2 months 1Ms 12
  ObsIDs: 8591 9593 9718 8593 8597 8595 8592 8596 9575 9578 8594 9596
  <P />III 2010.03-2010.07 4 months 2Ms 31 ObsIDs: 12043 12123 12044
  12128 12045 12129 12135 12046 12047 12137 12138 12055 12213 12048 12049
  12050 12222 12219 12051 12218 12223 12052 12220 12053 12054 12230 12231
  12227 12233 12232 12234 <P />IV 2014.06-2016.03 21 months 3Ms 48 ObsIDs:
  16183 16180 16456 16641 16457 16644 16463 17417 17416 16454 16176 16175
  16178 16177 16620 16462 17535 17542 16184 16182 16181 17546 16186 16187
  16188 16450 16190 16189 17556 16179 17573 17633 17634 16453 16451 16461
  16191 16460 16459 17552 16455 16458 17677 18709 18719 16452 18730 16185
  ---------------------------------------------------------------------------
  <P />(4 data files).

Title: Black Hole Growth Is Mainly Linked to Host-galaxy Stellar
    Mass Rather Than Star Formation Rate
Authors: Yang, G.; Chen, C. -T. J.; Vito, F.; Brandt, W. N.; Alexander,
   D. M.; Luo, B.; Sun, M. Y.; Xue, Y. Q.; Bauer, F. E.; Koekemoer,
   A. M.; Lehmer, B. D.; Liu, T.; Schneider, D. P.; Shemmer, O.; Trump,
   J. R.; Vignali, C.; Wang, J. -X.
Bibcode: 2017ApJ...842...72Y
Altcode: 2017arXiv170406658Y
  We investigate the dependence of black hole accretion rate (BHAR) on
  host-galaxy star formation rate (SFR) and stellar mass (M <SUB>*</SUB>)
  in the CANDELS/GOODS-South field in the redshift range of 0.5≤slant
  z&lt; 2.0. Our sample consists of ≈ {{18,000}} galaxies, allowing us
  to probe galaxies with 0.1{M}<SUB>⊙ </SUB>{{yr}}<SUP>-1</SUP>≲
  {SFR}≲ 100 {M}<SUB>⊙ </SUB> {{yr}}<SUP>-1</SUP> and/or
  {10}<SUP>8</SUP>{M}<SUB>⊙ </SUB>≲ {M}<SUB>* </SUB>≲
  {10}<SUP>11</SUP> {M}<SUB>⊙ </SUB>. We use sample-mean BHAR to
  approximate long-term average BHAR. Our sample-mean BHARs are derived
  from the Chandra Deep Field-South 7 Ms observations, while the SFRs
  and M <SUB>*</SUB> have been estimated by the CANDELS team through
  spectral energy distribution fitting. The average BHAR is correlated
  positively with both SFR and M <SUB>*</SUB>, and the BHAR-SFR and BHAR-M
  <SUB>*</SUB> relations can both be described acceptably by linear
  models with a slope of unity. However, BHAR appears to be correlated
  more strongly with M <SUB>*</SUB> than SFR. This result indicates
  that M <SUB>*</SUB> is the primary host-galaxy property related to
  supermassive black hole (SMBH) growth, and the apparent BHAR-SFR
  relation is largely a secondary effect due to the star-forming main
  sequence. Among our sources, massive galaxies ({M}<SUB>* </SUB>≳
  {10}<SUP>10</SUP>{M}<SUB>⊙ </SUB>) have significantly higher BHAR/SFR
  ratios than less massive galaxies, indicating that the former have
  higher SMBH fueling efficiency and/or higher SMBH occupation fraction
  than the latter. Our results can naturally explain the observed
  proportionality between {M}<SUB>{BH</SUB>} and M <SUB>*</SUB> for local
  giant ellipticals and suggest that their {M}<SUB>{BH</SUB>}/{M}<SUB>*
  </SUB> is higher than that of local star-forming galaxies. Among
  local star-forming galaxies, massive systems might have higher
  {M}<SUB>{BH</SUB>}/{M}<SUB>* </SUB> compared to dwarfs.

Title: Central Engine and Host Galaxy of RXJ 1301.9+2747:
    A Multiwavelength View of a Low-mass Black Hole Active Galactic
    Nuclei with Ultra-soft X-Ray Emission
Authors: Shu, X. W.; Wang, T. G.; Jiang, N.; Wang, J. X.; Sun, L. M.;
   Zhou, H. Y.
Bibcode: 2017ApJ...837....3S
Altcode: 2017arXiv170402886S
  RXJ 1301.9+2747 is an optically identified very-low-mass AGN
  candidate with {M}<SUB>{BH</SUB>}∼ 1× {10}<SUP>6</SUP> {M}<SUB>⊙
  </SUB>, which shows extremely soft X-ray emission and unusual X-ray
  variability in the form of short-lived flares. We present an analysis of
  multiwavelength observations of RXJ 1301.9+2747 in order to study the
  properties of the active nucleus and its host galaxy. The UV-to-X-ray
  spectrum in the quiescent state can be well and self-consistently
  described by a thermal and a Comptonized emission from the accretion
  disk, with the black body dominating ∼70% of the X-rays in the 0.2-2
  keV. The same model can describe the X-ray spectrum in the flare state,
  but the Comptonized component becomes dominant (∼80%). The best
  fit implies an Eddington ratio of ∼0.14 and a black-hole mass of
  (1.7-2.8)× {10}<SUP>6</SUP> M <SUB>⊙</SUB>, in agreement with
  the estimation from the optical data within errors. However, the
  best-fitting model under predicts the optical flux for the HST point
  source by a factor of ∼2. The excess of nuclear optical emission
  could be attributed to a nuclear stellar cluster, which is frequently
  seen in low-mass AGNs. The X-ray to optical spectral slope ({α
  }<SUB>{ox</SUB>}) is lower than in most other active galaxies, which may
  be attributed to intrinsically X-ray weakness due to very little hot
  and optically thin coronal emission. We performed a pilot search for
  weak or hidden broad emission lines using optical spectropolarimetry
  observations, but no polarized broad lines are detected. The host
  galaxy appears to be a disk galaxy with a boxy pseudobulge or nuclear
  bar accounting for ∼15% of the total starlight, which is consistent
  with the general characteristics of the host of low-mass AGNs.

Title: VizieR Online Data Catalog: Chandra Deep Field-South survey:
    7Ms sources (Luo+, 2017)
Authors: Luo, B.; Brandt, W. N.; Xue, Y. Q.; Lehmer, B.; Alexander,
   D. M.; Bauer, F. E.; Vito, F.; Yang, G.; Basu-Zych, A. R.; Comastri,
   A.; Gilli, R.; Gu, Q. -S.; Hornschemeier, A. E.; Koekemoer, A.; Liu,
   T.; Mainieri, V.; Paolillo, M.; Ranalli, P.; Rosati, P.; Schneider,
   D. P.; Shemmer, O.; Smail, I.; Sun, M.; Tozzi, P.; Vignali, C.; Wang,
   J. -X.
Bibcode: 2017yCat..22280002L
Altcode:
  The 7Ms CDF-S contains 102 Chandra ACIS-I observations, with a total
  cleaned exposure time of 6.727Ms, taken in four separate epochs of
  time. The basic information on these observations is listed in Table
  1. <P />There were 48 recent observations acquired between 2014 June
  9 and 2016 March 24, which constitute the last 3Ms of exposure of
  the 7Ms CDF-S. The first 1Ms of exposure consists of 11 observations
  taken between 1999 and 2000 (Giacconi+ 2002, J/ApJS/139/369; Rosati+
  2002ApJ...566..667R; Alexander+ 2003, J/AJ/126/539), the next 1Ms
  of exposure consists of 12 observations taken in 2007 (Luo+ 2008,
  J/ApJS/179/19), and another 2Ms of exposure includes 31 observations
  in 2010 (Xue+ 2011, J/ApJS/195/10). <P />The total area covered by
  the 7Ms CDF-S is 484.2arcmin<SUP>2</SUP>. <P />(3 data files).

Title: VizieR Online Data Catalog: 6Ms Chandra long-term analyses
    of AGNs (Yang+, 2016)
Authors: Yang, G.; Brandt, W. N.; Luo, B.; Xue, Y. Q.; Bauer, F. E.;
   Sun, M. Y.; Kim, S.; Schulze, S.; Zheng, X. C.; Paolillo, M.; Shemmer,
   O.; Liu, T.; Schneider, D. P.; Vignali, C.; Vito, F.; Wang, J. -X.
Bibcode: 2017yCat..18310145Y
Altcode:
  This work is based on the Chandra CDF-S data. The observations were
  taken from 1999 October to 2015 January with a total observation time
  of 5.7Ms. In total, there are 84 observations utilized with median
  exposure time ~60ks. All of the 84 observations were performed using the
  Advanced CCD Imaging Spectrometer imaging array (ACIS-I). See B. Luo
  et al. 2016, in prep (L16) for more observation details. Sixty-eight
  sources are selected with 649-11283 counts; the median number of counts
  is 1399. <P />(1 data file).

Title: The Chandra Deep Field-South Survey: 7 Ms Source Catalogs
Authors: Luo, B.; Brandt, W. N.; Xue, Y. Q.; Lehmer, B.; Alexander,
   D. M.; Bauer, F. E.; Vito, F.; Yang, G.; Basu-Zych, A. R.; Comastri,
   A.; Gilli, R.; Gu, Q. -S.; Hornschemeier, A. E.; Koekemoer, A.; Liu,
   T.; Mainieri, V.; Paolillo, M.; Ranalli, P.; Rosati, P.; Schneider,
   D. P.; Shemmer, O.; Smail, I.; Sun, M.; Tozzi, P.; Vignali, C.; Wang,
   J. -X.
Bibcode: 2017ApJS..228....2L
Altcode: 2016arXiv161103501L
  We present X-ray source catalogs for the ≈7 Ms exposure of the
  Chandra Deep Field-South (CDF-S), which covers a total area of 484.2
  arcmin<SUP>2</SUP>. Utilizing WAVDETECT for initial source detection and
  ACIS Extract for photometric extraction and significance assessment,
  we create a main source catalog containing 1008 sources that are
  detected in up to three X-ray bands: 0.5-7.0 keV, 0.5-2.0 keV, and
  2-7 keV. A supplementary source catalog is also provided, including 47
  lower-significance sources that have bright ({K}<SUB>s</SUB>≤slant 23)
  near-infrared counterparts. We identify multiwavelength counterparts
  for 992 (98.4%) of the main-catalog sources, and we collect redshifts
  for 986 of these sources, including 653 spectroscopic redshifts and
  333 photometric redshifts. Based on the X-ray and multiwavelength
  properties, we identify 711 active galactic nuclei (AGNs) from the
  main-catalog sources. Compared to the previous ≈4 Ms CDF-S catalogs,
  291 of the main-catalog sources are new detections. We have achieved
  unprecedented X-ray sensitivity with average flux limits over the
  central ≈1 arcmin<SUP>2</SUP> region of ≈1.9 × 10<SUP>-17</SUP>,
  6.4 × 10<SUP>-18</SUP>, and 2.7 × 10<SUP>-17</SUP> erg cm<SUP>-2</SUP>
  s<SUP>-1</SUP> in the three X-ray bands, respectively. We provide
  cumulative number-count measurements observing, for the first time,
  that normal galaxies start to dominate the X-ray source population at
  the faintest 0.5-2.0 keV flux levels. The highest X-ray source density
  reaches ≈50,500 deg<SUP>-2</SUP>, and 47% ± 4% of these sources
  are AGNs (≈23,900 deg<SUP>-2</SUP>).

Title: VizieR Online Data Catalog: LAMOST DR2 catalogs (Luo+, 2016)
Authors: Luo, A. -L.; Zhao, Y. -H.; Zhao, G.; Deng, L. -C.; Liu,
   X. -W.; Jing, Y. -P.; Wang, G.; Zhang, H. -T.; Shi, J. -R.; Cui,
   X. -Q.; Chu, Y. -Q.; Li, G. -P.; Bai, Z. -R.; Wu, Y.; Cai, Y.; Cao,
   S. -Y.; Cao, Z. -H.; Carlin, J. L.; Chen, H. -Y.; Chen, J. -J.; Chen,
   K. -X.; Chen, L.; Chen, X. -L.; Chen, X. -Y.; Chen, Y.; Christlieb,
   N.; Chu, J. -R.; Cui, C. -Z.; Dong, Y. -Q.; Du, B.; Fan, D. -W.; Feng,
   L.; Fu, J. -N.; Gao, P.; Gong, X. -F.; Gu, B. -Z.; Guo, Y. -X.; Han,
   Z. -W.; He, B. -L.; Hou, J. -L.; Hou, Y. -H.; Hou, W.; Hu, H. -Z.; Hu,
   N. -S.; Hu, Z. -W.; Huo, Z. -Y.; Jia, L.; Jiang, F. -H.; Jiang, X.;
   Jiang, Z. -B.; Jin, G.; Kong, X.; Kong, X.; Lei, Y. -J.; Li, A. -H.;
   Li, C. -H.; Li, G. -W.; Li, H. -N.; Li, J.; Li, Q.; Li, S.; Li, S. -S.;
   Li, X. -N.; Li, Y.; Li, Y. -B.; Li, Y. -P.; Liang, Y.; Lin, C. -C.;
   Liu, C.; Liu, G. -R.; Liu, G. -Q.; Liu, Z. -G.; Lu, W. -Z.; Luo, Y.;
   Mao, Y. -D.; Newberg, H.; Ni, J. -J.; Qi, Z. -X.; Qi, Y. -J.; Shen,
   S. -Y.; Shi, H. -M.; Song, J.; Song, Y. -H.; Su, D. -Q.; Su, H. -J.;
   Tang, Z. -H.; Tao, Q. -S.; Tian, Y.; Wang, D.; Wang, D. -Q.; Wang,
   F. -F.; Wang, G. -M.; Wang, H.; Wang, H. -C.; Wang, J.; Wang, J. -N.;
   Wang, J. -L.; Wang, J. -P.; Wang, J. -X.; Wang, L.; Wang, M. -X.;
   Wang, S. -G.; Wang, S. -Q.; Wang, X.; Wang, Y. -N.; Wang, Y.; Wang,
   Y. -F.; Wang, Y. -F.; Wei, P.; Wei, M. -Z.; Wu, H.; Wu, K. -F.; Wu,
   X. -B.; Wu, Y. -Z.; Xing, X. -Z.; Xu, L. -Z.; Xu, X. -Q.; Xu, Y.;
   Yan, T. -S.; Yang, D. -H.; Yang, H. -F.; Yang, H. -Q.; Yang, M.; Yao,
   Z. -Q.; Yu, Y.; Yuan, H.; Yuan, H. -B.; Yuan, H. -L.; Yuan, W. -M.;
   Zhai, C.; Zhang, E. -P.; Zhang, H. -W.; Zhang, J. -N.; Zhang, L. -P.;
   Zhang, W.; Zhang, Y.; Zhang, Y. -X.; Zhang, Z. -C.; Zhao, M.; Zhou,
   F.; Zhou, X.; Zhu, J.; Zhu, Y. -T.; Zou, S. -C.; Zuo, F.
Bibcode: 2016yCat.5149....0L
Altcode:
  There are a couple of corrections been made in this releasing:
  <P />Recalculated all the errors of Teff, Logg, Fe/H and rv in the
  AFGK catalog. Refer to the DR2 paper (in preparation) for details. <P
  />Compare to the previous internal releasing, some extra spectra has
  been added into this version of releasing: STAR from 3,779,597 to
  3,843,597, increased 63,923; GALAXY from 37,665 to 47,036, increased
  9,371; QSO from 8,633 to 13,262, increased 4,629. <P />The major
  contribution to this increasing is that we applied a new method to
  reduce the data which previously was abandoned due to lack of standard
  stars with high enough S/N. Refer to the paper 'LAMOST Spectrograph
  Response Curves: Stability and Application to flux calibration'
  (in preparation) for details. <P />There are also a small amount of
  increasing is due to the correction of fiber flag, and to the eye
  check work, etc. <P />(5 data files).

Title: The deepest X-ray view of high-redshift galaxies: constraints
    on low-rate black hole accretion
Authors: Vito, F.; Gilli, R.; Vignali, C.; Brandt, W. N.; Comastri,
   A.; Yang, G.; Lehmer, B. D.; Luo, B.; Basu-Zych, A.; Bauer, F. E.;
   Cappelluti, N.; Koekemoer, A.; Mainieri, V.; Paolillo, M.; Ranalli,
   P.; Shemmer, O.; Trump, J.; Wang, J. X.; Xue, Y. Q.
Bibcode: 2016MNRAS.463..348V
Altcode: 2016MNRAS.tmp.1093V; 2016arXiv160802614V
  We exploit the 7 Ms Chandra observations in the Chandra Deep Field-South
  (CDF-S), the deepest X-ray survey to date, coupled with CANDELS/GOODS-S
  data, to measure the total X-ray emission arising from 2076 galaxies at
  3.5 ≤ z &lt; 6.5. This aim is achieved by stacking the Chandra data
  at the positions of optically selected galaxies, reaching effective
  exposure times of ≥10<SUP>9</SUP>s. We detect significant (&gt;3.7σ)
  X-ray emission from massive galaxies at z ≈ 4. We also report the
  detection of massive galaxies at z ≈ 5 at a 99.7 per cent confidence
  level (2.7σ), the highest significance ever obtained for X-ray emission
  from galaxies at such high redshifts. No significant signal is detected
  from galaxies at even higher redshifts. The stacking results place
  constraints on the BHAD associated with the known high-redshift galaxy
  samples, as well as on the SFRD at high redshift, assuming a range of
  prescriptions for X-ray emission due to X- ray binaries. We find that
  the X-ray emission from our sample is likely dominated by processes
  related to star formation. Our results show that low-rate mass accretion
  on to SMBHs in individually X-ray-undetected galaxies is negligible,
  compared with the BHAD measured for samples of X-ray detected AGN, for
  cosmic SMBH mass assembly at high redshift. We also place, for the first
  time, constraints on the faint-end of the AGN X-ray luminosity function
  (logL<SUB>X</SUB> ∼ 42) at z &gt; 4, with evidence for fairly flat
  slopes. The implications of all of these findings are discussed in
  the context of the evolution of the AGN population at high redshift.

Title: Long-term X-Ray Variability of Typical Active Galactic Nuclei
    in the Distant Universe
Authors: Yang, G.; Brandt, W. N.; Luo, B.; Xue, Y. Q.; Bauer, F. E.;
   Sun, M. Y.; Kim, S.; Schulze, S.; Zheng, X. C.; Paolillo, M.; Shemmer,
   O.; Liu, T.; Schneider, D. P.; Vignali, C.; Vito, F.; Wang, J. -X.
Bibcode: 2016ApJ...831..145Y
Altcode: 2016arXiv160808224Y
  We perform long-term (≈15 years, observed-frame) X-ray variability
  analyses of the 68 brightest radio-quiet active galactic nuclei (AGNs)
  in the 6 Ms Chandra Deep Field-South survey; the majority are in the
  redshift range of 0.6-3.1, providing access to penetrating rest-frame
  X-rays up to ≈10-30 keV. Of the 68 sources, 24 are optical spectral
  type I AGNs, and the rest (44) are type II AGNs. The timescales probed
  in this work are among the longest for X-ray variability studies
  of distant AGNs. Photometric analyses reveal widespread photon flux
  variability: 90% of AGNs are variable above a 95% confidence level,
  including many X-ray obscured AGNs and several optically classified
  type II quasars. We characterize the intrinsic X-ray luminosity
  ({L}<SUB>{{X</SUB>}}) and absorption ({N}<SUB>{{H</SUB>}}) variability
  via spectral fitting. Most (74%) sources show {L}<SUB>{{X</SUB>}}
  variability; the variability amplitudes are generally smaller for
  quasars. A Compton-thick candidate AGN shows variability of its
  high-energy X-ray flux, indicating the size of reflecting material to be
  ≲0.3 pc. {L}<SUB>{{X</SUB>}} variability is also detected in a broad
  absorption line quasar. The {N}<SUB>{{H</SUB>}} variability amplitude
  for our sample appears to rise as time separation increases. About
  16% of sources show {N}<SUB>{{H</SUB>}} variability. One source
  transitions from an X-ray unobscured to obscured state, while its
  optical classification remains type I; this behavior indicates the
  X-ray eclipsing material is not large enough to obscure the whole
  broad-line region.

Title: Probing AGN Accretion History Through X-Ray Variability
Authors: Paolillo, Maurizio; Papadakis, I.; Brandt, W. N.; Xue, Y. Q.;
   Luo, B.; Tozzi, P.; Shemmer, O.; Allevato, V.; Bauer, F.; Koekemoer,
   A.; Vignali, C.; Vito, F.; Yang, G.; Wang, J. X.; Zheng, X.
Bibcode: 2016agnt.confE..39P
Altcode:
  I will present recent results on AGN variability in the CDFS
  survey. Using over 10 years of X-ray monitoring and comparison with
  local AGNs we are able to constrain the variability dependence on BH
  mass and accreton rate, and use it to trace the accretion hisory of
  the AGN population up to z=3.

Title: The Deepest X-Ray View Of High-Redshift Galaxies: Constraints
    On Low-Rate Black-Hole Accretion
Authors: Vito, Fabio; Gilli, R.; Vignali, C.; Brandt, W. N.; Comastri,
   A.; Yang, G.; Lehmer, B. D.; Luo, B.; Basu-Zych, A.; Bauer, F. E.;
   Cappelluti, N.; Koekemoer, A.; Mainieri, V.; Paolillo, M.; Ranalli,
   P.; Shemmer, O.; Trump, J.; Wang, J. X.
Bibcode: 2016agnt.confE..41V
Altcode:
  We exploit the new 7 Ms Chandra observations in the CDF-S, the deepest
  X-ray survey to date, coupled with CANDELS/GOODS- S data, to measure
  the total X-ray emission arising from 2000 galaxies at 3.5 &lt; z
  &lt; 6.5. This aim is achieved by stacking the Chandra data at the
  positions of optically selected galaxies, reaching effective exposure
  times of &gt;=10^9 s. We detect X-ray emission from z ∼ 4 galaxies
  at 3 ∼ 5sigma, while no significant signal is detected from galaxies
  at higher redshifts. The stacking results are used to estimate the
  black hole accretion rate density (BHAD) and star -formation rate
  density (SFRD) at high redshift, assuming a range of prescriptions
  for X-ray emission due to X-ray binaries. We find that X-ray emission
  from our sample is likely dominated by processes related to star
  formation. Our results show that low-rate mass accretion onto SMBHs in
  individually X-ray-undetected galaxies is negligible, compared with
  the BHAD measured for samples of X-ray detected AGN, for cosmic SMBH
  mass assembly at high redshift. We also place, for the first time,
  constraints on the faint-end of the AGN X- ray luminosity function
  (logLX ∼ 42) at z &gt; 4, with evidence for fairly flat slopes.

Title: VizieR Online Data Catalog: Evolution of ~6Ms CDF-S galaxies
    (Lehmer+, 2016)
Authors: Lehmer, B. D.; Basu-Zych, A. R.; Mineo, S.; Brandt, W. N.;
   Eufrasio, R. T.; Fragos, T.; Hornschemeier, A. E.; Luo, B.; Xue,
   Y. Q.; Bauer, F. E.; Gilfanov, M.; Ranalli, P.; Schneider, D. P.;
   Shemmer, O.; Tozzi, P.; Trump, J. R.; Vignali, C.; Wang, J. -X.;
   Yukita, M.; Zezas, A.
Bibcode: 2016yCat..18250007L
Altcode:
  We began with an initial sample of 32508 galaxies in the Great
  Observatories Origins Deep Survey South (GOODS-S) footprint as presented
  in Section 2 of Xue et al. (2012, J/ApJ/758/129). We cut our initial
  sample to the 24941 objects that were within 7' of the mean ~6Ms CDF-S
  aimpoint, a region where the Chandra point-spread function (PSF) is
  sharpest and the corresponding X-ray sensitivity is highest. See text
  for further explanations. <P />(2 data files).

Title: The Evolution of Normal Galaxy X-Ray Emission through Cosmic
History: Constraints from the 6 MS Chandra Deep Field-South
Authors: Lehmer, B. D.; Basu-Zych, A. R.; Mineo, S.; Brandt, W. N.;
   Eufrasio, R. T.; Fragos, T.; Hornschemeier, A. E.; Luo, B.; Xue,
   Y. Q.; Bauer, F. E.; Gilfanov, M.; Ranalli, P.; Schneider, D. P.;
   Shemmer, O.; Tozzi, P.; Trump, J. R.; Vignali, C.; Wang, J. -X.;
   Yukita, M.; Zezas, A.
Bibcode: 2016ApJ...825....7L
Altcode: 2016arXiv160406461L
  We present measurements of the evolution of normal-galaxy X-ray
  emission from z\quad ≈ 0-7 using local galaxies and galaxy samples
  in the ≈6 Ms Chandra Deep Field-South (CDF-S) survey. The majority
  of the CDF-S galaxies are observed at rest-frame energies above 2
  keV, where the emission is expected to be dominated by X-ray binary
  (XRB) populations; however, hot gas is expected to provide small
  contributions to the observed-frame ≲1 keV emission at z ≲
  1. We show that a single scaling relation between X-ray luminosity
  ({L}<SUB>{{X</SUB>}}) and star-formation rate (SFR) literature,
  is insufficient for characterizing the average X-ray emission at all
  redshifts. We establish that scaling relations involving not only SFR,
  but also stellar mass ({M}<SUB>\star </SUB>) and redshift, provide
  significantly improved characterizations of the average X-ray emission
  from normal galaxy populations at z\quad ≈ 0-7. We further provide the
  first empirical constraints on the redshift evolution of X-ray emission
  from both low-mass XRB (LMXB) and high-mass XRB (HMXB) populations and
  their scalings with {M}<SUB>\star </SUB> and SFR, respectively. We
  find {L}<SUB>2-10{keV</SUB>}(LMXB)/{M}<SUB>\star </SUB>\propto
  {(1+z)}<SUP>2-3</SUP> and {L}<SUB>2-10{keV</SUB>}(HMXB)/SFR \propto
  \quad (1+z), and show that these relations are consistent with XRB
  population-synthesis model predictions, which attribute the increase in
  LMXB and HMXB scaling relations with redshift as being due to declining
  host galaxy stellar ages and metallicities, respectively. We discuss
  how emission from XRBs could provide an important source of heating
  to the intergalactic medium in the early universe, exceeding that of
  active galactic nuclei.

Title: Observations of Magnetic Flux-rope Oscillation during the
    Precursor Phase of a Solar Eruption
Authors: Zhou, G. P.; Zhang, J.; Wang, J. X.
Bibcode: 2016ApJ...823L..19Z
Altcode:
  Based on combined observations from the Interface Region Imaging
  Spectrograph (IRIS) spectrometer with the coronal emission line
  of Fe xxi at 1354.08 Å and SDO/AIA images in multiple passbands,
  we report the finding of the precursor activity manifested as the
  transverse oscillation of a sigmoid, which is likely a pre-existing
  magnetic flux rope (MFR), that led to the onset of an X class flare
  and a fast halo coronal mass ejection (CME) on 2014 September 10. The
  IRIS slit is situated at a fixed position that is almost vertical
  to the main axis of the sigmoid structure that has a length of about
  1.8 × 10<SUP>5</SUP> km. This precursor oscillation lasts for about
  13 minutes in the MFR and has velocities in the range of [-9, 11] km
  s<SUP>-1</SUP> and a period of ∼280 s. Our analysis, which is based
  on the temperature, density, length, and magnetic field strength of
  the observed sigmoid, indicates that the nature of the oscillation is a
  standing wave of fast magnetoacoustic kink mode. We further find that
  the precursor oscillation is excited by the energy released through
  an external magnetic reconnection between the unstable MFR and the
  ambient magnetic field. It is proposed that this precursor activity
  leads to the dynamic formation of a current sheet underneath the MFR
  that subsequently reconnects to trigger the onset of the main phase
  of the flare and the CME.

Title: Identification of z ≳ 2 Herschel 500 μM Sources Using
    Color Deconfusion
Authors: Shu, X. W.; Elbaz, D.; Bourne, N.; Schreiber, C.; Wang, T.;
   Dunlop, J. S.; Fontana, A.; Leiton, R.; Pannella, M.; Okumura, K.;
   Michałowski, M. J.; Santini, P.; Merlin, E.; Buitrago, F.; Bruce,
   V. A.; Amorin, R.; Castellano, M.; Derriere, S.; Comastri, A.;
   Cappelluti, N.; Wang, J. X.; Ferguson, H. C.
Bibcode: 2016ApJS..222....4S
Altcode: 2015arXiv151200167S
  We present a new method to search for candidate z ≳ 2 Herschel 500
  μm sources in the Great Observatories Origins Deep Survey-North field
  using a S<SUB>500 μm</SUB>/S<SUB>24 μm</SUB> “color deconfusion”
  technique. Potential high-z sources are selected against low-redshift
  ones from their large 500 to 24 μm flux density ratios. By effectively
  reducing the contribution from low-redshift populations to the
  observed 500 μm emission, we are able to identify counterparts to
  high-z 500 μm sources whose 24 μm fluxes are relatively faint. The
  recovery of known z ≳ 4 starbursts confirms the efficiency of this
  approach in selecting high-z Herschel sources. The resulting sample
  consists of 34 dusty star-forming galaxies at z ≳ 2. The inferred
  infrared luminosities are in the range 1.5 × 10<SUP>12</SUP>-1.8 ×
  10<SUP>13</SUP> L<SUB>⊙</SUB>, corresponding to dust-obscured star
  formation rates (SFRs) of ∼260-3100 M<SUB>⊙</SUB> yr<SUP>-1</SUP>
  for a Salpeter initial mass function. Comparison with previous SCUBA 850
  μ {{m}}-selected galaxy samples shows that our method is more efficient
  at selecting high-z dusty galaxies, with a median redshift of z=3.07+/-
  0.83 and with 10 of the sources at z ≳ 4. We find that at a fixed
  luminosity, the dust temperature is ∼5 K cooler than that expected
  from the {T}<SUB>d</SUB>-{L}<SUB>{{IR</SUB>}} relation at z\quad ≲ 1,
  though different temperature selection effects should be taken into
  account. The radio-detected subsample (excluding three strong active
  galactic nucleus) follows the far-infrared (far-IR)/radio correlation at
  lower redshifts, and no evolution with redshift is observed out to z∼
  5, suggesting that the far-IR emission is star formation dominated. The
  contribution of the high-z Herschel 500 μm sources to the cosmic SFR
  density is comparable to that of (sub)millimeter galaxy populations at
  z∼ 2.5 and at least 40% of the extinction-corrected UV samples at
  z∼ 4. Further investigation into the nature of these high-z dusty
  galaxies will be crucial for our understanding of the star formation
  histories and the buildup of stellar mass at the earliest cosmic epochs.

Title: Photometric Redshifts in the Hawaii-Hubble Deep Field-North
Authors: Yang, G.; Xue, Y. Q.; Luo, B.; Brandt, W. N.; Alexander,
   D. M.; Bauer, F. E.; Cui, W.; Kong, X.; Lehmer, B. D.; Wang, J. -X.;
   Wu, X. -B.; Yuan, F.; Yuan, Y. -F.; Zhou, H. Y.
Bibcode: 2016IAUS..319...56Y
Altcode:
  We derive z <SUB>phot</SUB> for sources in the entire (~0.4
  deg<SUP>2</SUP>) H-HDF-N field with the EAzY code, based on PSF-matched
  broad-band (U band to IRAC 4.5 μm) photometry. Our catalog consists
  of a total of 131,678 sources. We find σ<SUB>NMAD</SUB> = 0.029 for
  non-X-ray sources. We also classify each object as a star or galaxy
  through SED fitting. Furthermore, we match our catalog with the 2 Ms
  CDF-N main X-ray catalog. For the 462 matched non-stellar X-ray sources,
  we improve their z <SUB>phot</SUB> quality (σ<SUB>NMAD</SUB> = 0.035)
  by adding three additional AGN templates. We make our photometry and
  z <SUB>phot</SUB> catalog publicly available.

Title: VizieR Online Data Catalog: LAMOST DR1 catalogs (Luo+, 2015)
Authors: Luo, A. -L.; Zhao, Y. -H.; Zhao, G.; Deng, L. -C.; Liu,
   X. -W.; Jing, Y. -P.; Wang, G.; Zhang, H. -T.; Shi, J. -R.; Cui,
   X. -Q.; Chu, Y. -Q.; Li, G. -P.; Bai, Z. -R.; Wu, Y.; Cai, Y.; Cao,
   S. -Y.; Cao, Z. -H.; Carlin, J. L.; Chen, H. -Y.; Chen, J. -J.; Chen,
   K. -X.; Chen, L.; Chen, X. -L.; Chen, X. -Y.; Chen, Y.; Christlieb,
   N.; Chu, J. -R.; Cui, C. -Z.; Dong, Y. -Q.; Du, B.; Fan, D. -W.; Feng,
   L.; Fu, J. -N.; Gao, P.; Gong, X. -F.; Gu, B. -Z.; Guo, Y. -X.; Han,
   Z. -W.; He, B. -L.; Hou, J. -L.; Hou, Y. -H.; Hou, W.; Hu, H. -Z.; Hu,
   N. -S.; Hu, Z. -W.; Huo, Z. -Y.; Jia, L.; Jiang, F. -H.; Jiang, X.;
   Jiang, Z. -B.; Jin, G.; Kong, X.; Kong, X.; Lei, Y. -J.; Li, A. -H.;
   Li, C. -H.; Li, G. -W.; Li, H. -N.; Li, J.; Li, Q.; Li, S.; Li, S. -S.;
   Li, X. -N.; Li, Y.; Li, Y. -B.; Li, Y. -P.; Liang, Y.; Lin, C. -C.;
   Liu, C.; Liu, G. -R.; Liu, G. -Q.; Liu, Z. -G.; Lu, W. -Z.; Luo,
   Y.; Mao, Y. -D.; Newberg, H.; Ni, J. -J.; Qi, Z. -X.; Qi, Y. -J.;
   Shen, S. -Y.; Shi, H. -M.; Song, J.; Song, Y. -H.; Su, D. -Q.; Su,
   H. -J.; Tang, Z. -H.; Tao, Q. -S.; Tian, Y.; Wang, D.; Wang, D. -Q.;
   Wang, F. -F.; Wang, G. -M.; Wang, H.; Wang, H. -C.; Wang, J.; Wan!,
   G. J. -N.; Wang, J. -L.; Wang, J. -P.; Wang, J. -X.; Wang, L.; Wang,
   M. -X.; Wang, S. -G.; Wang, S. -Q.; Wang, X.; Wang, Y. -N.; Wang, Y.;
   Wang, Y. -F.; Wang, Y. -F.; Wei, P.; Wei, M. -Z.; Wu, H.; Wu, K. -F.;
   Wu, X. -B.; Wu, Y. -Z.; Xing, X. -Z.; Xu, L. -Z.; Xu, X. -Q.; Xu, Y.;
   Yan, T. -S.; Yang, D. -H.; Yang, H. -F.; Yang, H. -Q.; Yang, M.; Yao,
   Z. -Q.; Yu, Y.; Yuan, H.; Yuan, H. -B.; Yuan, H. -L.; Yuan, W. -M.;
   Zhai, C.; Zhang, E. -P.; Zhang, H. -W.; Zhang, J. -N.; Zhang, L. -P.;
   Zhang, W.; Zhang, Y.; Zhang, Y. -X.; Zhang, Z. -C.; Zhao, M.; Zhou,
   F.; Zhou, X.; Zhu, J.; Zhu, Y. -T.; Zou, S. -C.; Zuo, F.
Bibcode: 2015yCat.5146....0L
Altcode:
  The LAMOST general catalog includes 717469 objects obtained from the
  LAMOST pilot survey, which contain 648746 stars, 2723 galaxies, 621
  quasars and 65406 unknown objects, and 1487200 objects obtained from
  the LAMOST general survey, which contain 1295583 stars, 9359 galaxies,
  4396 quasars and 177862 unknown objects, so this catalog totally
  includes 2204696 objects including 1,944,329 stars, 12082 galaxies,
  5017 quasars and 243268 unknown objects. In this catalog, there are
  1186132 objects with SNR of g band larger than 10, 1680794 objects with
  SNR of i band larger than 10, and 1746202 objects with SNR of g band
  larger than 10 and SNR of i band larger than 10. <P />(6 data files).

Title: Does the Variation of Solar Intra-network Horizontal Field
    Follow Sunspot Cycle?
Authors: Jin, C. L.; Wang, J. X.
Bibcode: 2015ApJ...807...70J
Altcode:
  The ubiquitousness of the solar inter-network horizontal magnetic
  field has been revealed by space-borne observations with high spatial
  resolution and polarization sensitivity. However, no consensus has
  been achieved on the origin of the horizontal field among solar
  physicists. For a better understanding, in this study, we analyze
  the cyclic variation of the inter-network horizontal field by using
  the spectro-polarimeter observations provided by the Solar Optical
  Telescope on board Hinode, covering the interval from 2008 April
  to 2015 February. The method of wavelength integration is adopted to
  achieve a high signal-to-noise ratio. It is found that from 2008 to 2015
  the inter-network horizontal field does not vary when solar activity
  increases, and the average flux density of the inter-network horizontal
  field is 87 ± 1 G, In addition, the imbalance between horizontal and
  vertical fields also keeps invariant within the scope of deviation,
  i.e., 8.7 ± 0.5, from the solar minimum to maximum of solar cycle
  24. This result confirms that the inter-network horizontal field is
  independent of the sunspot cycle. The revelation favors the idea that
  a local dynamo is creating and maintaining the solar inter-network
  horizontal field.

Title: VizieR Online Data Catalog: SWXCS III. Cluster catalog from
    2005-2012 Swift data (Liu+, 2015)
Authors: Liu, T.; Tozzi, P.; Tundo, E.; Moretti, A.; Rosati, P.;
   Wang, J. -X.; Tagliaferri, G.; Campana, S.; Giavalisco, M.
Bibcode: 2015yCat..22160028L
Altcode:
  From the entire Swift XRT archive in the period 2005 February-2012
  November, we select all the fields that can be used to build an
  unbiased, serendipitous X-ray cluster catalog. <P />(2 data files).

Title: VizieR Online Data Catalog: Photometric redshifts in the
    Hawaii-HDF-N (Yang+, 2014)
Authors: Yang, G.; Xue, Y. Q.; Luo, B.; Brandt, W. N.; Alexander,
   D. M.; Bauer, F. E.; Cui, W.; Kong, X.; Lehmer, B. D.; Wang, J. -X.;
   Wu, X. -B.; Yuan, F.; Yuan, Y. -F.; Zhou, H. Y.
Bibcode: 2015yCat..22150027Y
Altcode:
  We collect the U-, B-, V-, R-, I-, z'-, and HK'-band images from
  Capak+, 2004, J/AJ/127/180, the J- and H-band images from Keenan et
  al. (2010ApJS..186...94K), and the Ks-band image from Wang et al. (2010,
  J/ApJS/187/251), respectively. We also make use of an independently
  observed z'-band image from Ouchi et al. (2009ApJ...706.1136O). The
  IRAC 3.6, 4.5, 5.8, and 8.0um images were obtained from the Spitzer
  Heritage Archive, while another set of IRAC 3.6 and 4.5um images were
  taken from the Spitzer Extended Deep Survey (SEDS) presented in Ashby
  et al. (2013, J/ApJ/769/80). <P />(1 data file).

Title: Photometric Redshifts in the Hawaii-Hubble Deep Field-North
    (H-HDF-N)
Authors: Yang, G.; Xue, Y. Q.; Luo, B.; Brandt, W. N.; Alexander,
   D. M.; Bauer, F. E.; Cui, W.; Kong, X.; Lehmer, B. D.; Wang, J. -X.;
   Wu, X. -B.; Yuan, F.; Yuan, Y. -F.; Zhou, H. Y.
Bibcode: 2014ApJS..215...27Y
Altcode: 2014arXiv1410.6860Y
  We derive photometric redshifts (z <SUB>phot</SUB>) for sources in the
  entire (~0.4 deg<SUP>2</SUP>) Hawaii-Hubble Deep Field-North (H-HDF-N)
  field with the EAzY code, based on point-spread-function-matched
  photometry of 15 broad bands from the ultraviolet (U band) to
  mid-infrared (IRAC 4.5 μm). Our catalog consists of a total of 131,678
  sources. We evaluate the z <SUB>phot</SUB> quality by comparing z
  <SUB>phot</SUB> with spectroscopic redshifts (z <SUB>spec</SUB>) when
  available, and find a value of normalized median absolute deviation
  σ<SUB>NMAD</SUB> = 0.029 and an outlier fraction of 5.5% (outliers are
  defined as sources having |z<SUB>phot</SUB> - z<SUB>spec</SUB> |/(1 +
  z<SUB>spec</SUB> ) &gt; 0.15) for non-X-ray sources. More specifically,
  we obtain σ<SUB>NMAD</SUB> = 0.024 with 2.7% outliers for sources
  brighter than R = 23 mag, σ<SUB>NMAD</SUB> = 0.035 with 7.4% outliers
  for sources fainter than R = 23 mag, σ<SUB>NMAD</SUB> = 0.026 with 3.9%
  outliers for sources having z &lt; 1, and σ<SUB>NMAD</SUB> = 0.034 with
  9.0% outliers for sources having z &gt; 1. Our z <SUB>phot</SUB> quality
  shows an overall improvement over an earlier z <SUB>phot</SUB> work
  that focused only on the central H-HDF-N area. We also classify each
  object as a star or galaxy through template spectral energy distribution
  fitting and complementary morphological parameterization, resulting
  in 4959 stars and 126,719 galaxies. Furthermore, we match our catalog
  with the 2 Ms Chandra Deep Field-North main X-ray catalog. For the
  462 matched non-stellar X-ray sources (281 having z <SUB>spec</SUB>),
  we improve their z <SUB>phot</SUB> quality by adding three additional
  active galactic nucleus templates, achieving σ<SUB>NMAD</SUB> =
  0.035 and an outlier fraction of 12.5%. We make our catalog publicly
  available presenting both photometry and z <SUB>phot</SUB>, and provide
  guidance on how to make use of our catalog.

Title: The Swift X-ray Cluster Survey
Authors: Moretti, A.; Wang, J. X.; Liu, T.; Tundo, E.; Giavalisco,
   M.; Liu, T.; Tozzi, P.; Campana, S.; Tagliaferri, G.
Bibcode: 2014styd.confE..43M
Altcode: 2014PoS...233E..43M
  No abstract at ADS

Title: Variation of the solar magnetic flux spectrum during solar
    cycle 23
Authors: Jin, C. L.; Wang, J. X.
Bibcode: 2014JGRA..119...11J
Altcode: 2013arXiv1312.5816J
  By using the unique database of Solar and Heliospheric
  Observatory/Michelson Doppler Imager full disk magnetograms from
  September 1996 to January 2011, covering the entire solar cycle 23,
  we analyze the time-variability of the solar magnetic flux spectrum
  and study the properties of extended minimum of cycle 23. We totally
  identify 11.5 million magnetic structures. It has been revealed
  that magnetic features with different magnetic fluxes exhibit
  different cycle behaviors. The magnetic features with flux larger
  than 4.0×10<SUP>19</SUP> Mx, which cover solar active regions and
  strong network features, show exactly the same variation as sunspots;
  however, the remaining 82% magnetic features which cover the majority of
  network elements show anti-phase variation with sunspots. We select a
  criterion that the monthly sunspot number is less than 20 to represent
  the Sun's low activity status. Then we find the extended minimum of
  cycle 23 is characterized by the long duration of low activity status,
  but the magnitude of magnetic flux in this period is not lower than
  previous cycle. Both the duration of low activity status and the minimum
  activity level defined by minimum sunspot number show a century period
  approximately. The extended minimum of cycle 23 shows similarities
  with solar cycle 11, which preceded the mini-maxima in later solar
  cycles. This similarity is suggestive that the solar cycles following
  cycle 23 are likely to have low activity.

Title: Formation and disappearance of a filament
Authors: Zhou, G. P.; Wang, J. X.; Tsuneta, S.
Bibcode: 2013IAUS..294..593Z
Altcode:
  A continuous observations near an small active region (AR) NOAA 10976
  by the Solar Optical Telescope (SOT) and X-Ray Telescope (XRT) on board
  the Hinode satellite during Dec. 02 2007 from 15:50 UT to 19:59 UT. We
  observed that: (a) the filament formed by merging parallel fibrils into
  a twist structure. (b) the filament faded by reconnecting among its
  own loop structures, or being stripped into pieces.These process are
  always preceded by the brightening. (c) for the disappearance of the
  filament, it has close correlation with the activity, like untwisting
  or expanding, of its corresponding X-ray bright rope.

Title: The Swift X-Ray Cluster Survey
Authors: Liu, T.; Tozzi, P.; Moretti, A.; Tundo, E.; Rosati, P.;
   Borgani, S.; Tagliaferri, G.; Capana, S.; Fugazza, D.; D'Avanzo, P.;
   Wang, J. -X.; Guglielmetti, F.
Bibcode: 2013tcec.confE..28L
Altcode:
  No abstract at ADS

Title: EXSdetect: an end-to-end software for extended source detection
in X-ray images: application to Swift-XRT data
Authors: Liu, T.; Tozzi, P.; Tundo, E.; Moretti, A.; Wang, J. -X.;
   Rosati, P.; Guglielmetti, F.
Bibcode: 2013A&A...549A.143L
Altcode: 2012arXiv1212.4038L
  <BR /> Aims: We present a stand-alone software (named EXSdetect)
  for the detection of extended sources in X-ray images. Our goal is to
  provide a flexible tool capable of detecting extended sources down to
  the lowest flux levels attainable within instrumental limitations,
  while maintaining robust photometry, high completeness, and low
  contamination, regardless of source morphology. EXSdetect was developed
  mainly to exploit the ever-increasing wealth of archival X-ray data,
  but is also ideally suited to explore the scientific capabilities of
  future X-ray facilities, with a strong focus on investigations of
  distant groups and clusters of galaxies. <BR /> Methods: EXSdetect
  combines a fast Voronoi tessellation code with a friends-of-friends
  algorithm and an automated deblending procedure. The values of key
  parameters are matched to fundamental telescope properties such as
  angular resolution and instrumental background. In addition, the
  software is designed to permit extensive tests of its performance
  via simulations of a wide range of observational scenarios. <BR />
  Results: We applied EXSdetect to simulated data fields modeled to
  realistically represent the Swift X-ray Cluster Survey (SXCS), which
  is based on archival data obtained by the X-ray telescope onboard the
  Swift satellite. We achieve more than 90% completeness for extended
  sources comprising at least 80 photons in the 0.5-2 keV band, a limit
  that corresponds to 10<SUP>-14</SUP> erg cm<SUP>-2</SUP> s<SUP>-1</SUP>
  for the deepest SXCS fields. This detection limit is comparable to the
  one attained by the most sensitive cluster surveys conducted with much
  larger X-ray telescopes. While evaluating the performance of EXSdetect,
  we also explored the impact of improved angular resolution and discuss
  the ideal properties of the next generation of X-ray survey missions. <P
  />The Phyton code EXSdetect is available on the SXCS website <A
  href="http://adlibitum.oats.inaf.it/sxcs">http://adlibitum.oats.inaf.it/sxcs</A>

Title: Solar Intranetwork Magnetic Elements: Intrinsically Weak
    or Strong?
Authors: Jin, C. L.; Wang, J. X.; Xie, Z. X.
Bibcode: 2012SoPh..280...51J
Altcode: 2012SoPh..tmp..151J
  The high spatial resolution observation of a quiet region taken with
  the Solar Optical Telescope/Spectro-Polarimeter aboard the Hinode
  spacecraft is analyzed. Based on the Milne-Eddington atmospheric
  model, the vector magnetic field of the quiet region is derived by
  fitting the full Stokes profiles of the Fe I 630 nm line pair. We
  extract intranetwork (IN) region from the quiet region and identify
  5058 IN magnetic elements, and study their magnetic properties. As a
  comparison, the magnetic properties of network (NT) region are also
  analyzed. The main results are as follows. i) The IN area displays a
  predominance of weak (hecto-gauss) field concentration, i.e., 99.8 %
  of IN area shows the weak field. Moreover, the vector magnetic field
  exhibits concentration toward horizontal direction. However, for
  the NT region, we discover the coexistence of weak field and strong
  (kilo-gauss, kG) field. In the IN and NT regions, the filling factor
  shows almost the same probability distribution function with the peak
  at about 0.28. ii) All IN magnetic elements show field strength less
  than 1 kG. However, some NT elements display the coexistence of weak
  field and strong field. Regardless of NT or IN elements, about 20 %
  of elements lies in the Doppler blue-shift region. Our results imply
  that not all magnetic elements lie in the down-draft sites.

Title: Quantifying solar superactive regions with vector magnetic
    field observations
Authors: Chen, A. Q.; Wang, J. X.
Bibcode: 2012A&A...543A..49C
Altcode: 2012arXiv1205.6533C
  Context. The vector magnetic field characteristics of superactive
  regions (SARs) hold the key for understanding why SARs are extremely
  active and provide the guidance in space weather prediction. <BR />
  Aims: We aim to quantify the characteristics of SARs using the vector
  magnetograms taken by the Solar Magnetic Field Telescope at Huairou
  Solar Observatory Station. <BR /> Methods: The vector magnetic field
  characteristics of 14 SARs in solar cycles 22 and 23 were analyzed
  using the following four parameters: 1) the magnetic flux imbalance
  between opposite polarities; 2) the total photospheric free magnetic
  energy; 3) the length of the magnetic neutral line with its steep
  horizontal magnetic gradient; and 4) the area with strong magnetic
  shear. Furthermore, we selected another eight large and inactive active
  regions (ARs), which are called fallow ARs (FARs), to compare them
  with the SARs. <BR /> Results: We found that most of the SARs have
  a net magnetic flux higher than 7.0 × 10<SUP>21</SUP> Mx, a total
  photospheric free magnetic energy higher than 1.0 × 10<SUP>24</SUP>
  erg cm<SUP>-1</SUP>, a magnetic neutral line with a steep horizontal
  magnetic gradient (≥300 G Mm<SUP>-1</SUP>) longer than 30 Mm, and
  an area with strong magnetic shear (shear angle ≥ 80°) greater
  than 100 Mm<SUP>2</SUP>. In contrast, the values of these parameters
  for the FARs are mostly very low. The Pearson χ<SUP>2</SUP> test was
  used to examine the significance of the difference between the SARs
  and FARs, and the results indicate that these two types of ARs can
  be fairly distinguished by each of these parameters. The significance
  levels are 99.55%, 99.98%, 99.98%, and 99.96%, respectively. However,
  no single parameter can distinguish them perfectly. Therefore we
  propose a composite index based on these parameters, and find that
  the distinction between the two types of ARs is also significant with
  a significance level of 99.96%. These results are useful for a better
  physical understanding of the SAR and FAR.

Title: Sun's small-scale magnetic field : from quiet region to
    polar region
Authors: Jin, C. L.; Wang, J. X.; Zhao, M.
Bibcode: 2012EAS....55...15J
Altcode:
  In this contribution, we present our recent effort in understanding
  the solar small-scale magnetic field. Firstly, with the unique
  data from MDI/SOHO in an interval embodying solar cycle 23, we find
  three categories of small-scale magnetic elements, and their number
  variations shows no correlation, anti-correlation and correlation
  with sunspots, respectively. The possible sources for the three
  categories of small-scale magnetic elements are discussed. Secondly,
  by the observations from SOT on board Hinode, we study the properties
  of vector magnetic field in quiet Sun. The following results are
  summarized. (1) Two categories of horizontal magnetic elements are
  disclosed, and most of horizontal elements are associate with the
  emergence of U-loop. (2) The magnetic field of quiet region is obviously
  non-potential. The filigrees and network bright points are characterized
  by strong longitudinal field, large electric helicity and free energy
  density. (3) For quiet region, the intra-network region displays a
  predominance of weak field concentration, but network region shows
  the coexisting of weak field with strong field; For polar region,
  the strong field occupies 6.7% of the region. (4) On quiet region,
  the magnetic field mainly resides in the inter-granular lanes. By the
  observation, we reconstruct an average granular model, for which the
  detailed distributions of vector fields, Doppler velocity and intensity
  are obtained.

Title: Revision of Solar Spicule Classification
Authors: Zhang, Y. Z.; Shibata, K.; Wang, J. X.; Mao, X. J.; Matsumoto,
   T.; Liu, Y.; Su, J. T.
Bibcode: 2012ApJ...750...16Z
Altcode: 2012arXiv1202.4518Z
  Solar spicules are the fundamental magnetic structures in the
  chromosphere and may play a key role in channeling the chromosphere and
  corona. Recently, it was suggested by De Pontieu et al. that there were
  two types of spicules with very different dynamic properties, which were
  detected by the space-time plot technique in the Ca II H line (3968 Å)
  wavelength from Hinode/Solar Optical Telescope observations. A "Type
  I" spicule with a 3-7-minute lifetime undergoes a cycle of upward and
  downward motions; by contrast, a "Type II" spicule fades away within
  dozens of seconds without a descending phase. We are motivated by the
  fact that for a spicule with complicated three-dimensional motion the
  space-time plot, which is made through a slit on a fixed position, could
  not match the spicule behavior all the time and might lose its real life
  story. By revisiting the same data sets, we identify and trace 105 and
  102 spicules in the quiet Sun (QS) and coronal hole (CH), respectively,
  and obtain their statistical dynamic properties. First, we have not
  found a single convincing example of "Type II" spicules. Second, more
  than 60% of the identified spicules in each region show a complete
  cycle, i.e., the majority are "Type I" spicules. Third, the lifetimes
  of the spicules in the QS and CH are 148 s and 112 s, respectively,
  but there is no fundamental lifetime difference between the spicules
  in the QS and CH reported earlier. Therefore, the suggestion of coronal
  heating by "Type II" spicules should be taken with caution.

Title: A Possible Ultra Strong and Broad Fe Kα Emission Line in
    Seyfert 2 Galaxy IRAS 00521-7054
Authors: Tan, Y.; Wang, J. X.; Shu, X. W.; Zhou, Youyuan
Bibcode: 2012ApJ...747L..11T
Altcode: 2012arXiv1202.0400T
  We present XMM-Newton spectra of the Seyfert 2 Galaxy IRAS 00521-7054. A
  strong feature at ~6 keV (observer's frame) can be formally fitted with
  a strong (EW = 1.3 ± 0.3 keV in the rest frame) and broad Fe Kα line,
  extending down to 3 keV. The underlying X-ray continuum could be fitted
  with an absorbed power law (with Γ = 1.8 ± 0.2 and N <SUB>H</SUB> =
  5.9<SUP>+0.6</SUP> <SUB>-0.7</SUB> × 10<SUP>22</SUP> cm<SUP>-2</SUP>)
  plus a soft component. If due to relativistically smeared reflection by
  an X-ray illuminated accretion disk, the spin of the supermassive black
  hole (SMBH) is constrained to be 0.97<SUP>+0.03</SUP> <SUB>-0.13</SUB>
  (errors at 90% confidence level for one interesting parameter), and the
  accretion system is viewed at an inclination angle of 37° ± 4°. This
  would be the first type 2 active galactic nucleus reported with strong
  red Fe Kα wing detected which demands a fast rotating SMBH. The
  unusually large EW would suggest that the light bending effect is
  strong in this source. Alternatively, the spectra could be fitted by
  a dual-absorber model (though with a global χ<SUP>2</SUP> higher by
  ~6 for 283 dof) with N <SUB>H1</SUB> = 7.0 ± 0.8 × 10<SUP>22</SUP>
  cm<SUP>-2</SUP> covering 100% of the X-ray source, and N <SUB>H2</SUB>
  = 21.7<SUP>+5.6</SUP> <SUB>-5.4</SUB> × 10<SUP>22</SUP> cm<SUP>-2</SUP>
  covering 71%, which does not require an extra broad Fe Kα line.

Title: On the X-Ray Baldwin Effect in Active Galactic Nuclei Observed
    by the Chandra High-energy Grating
Authors: Shu, X. W.; Wang, J. X.; Yaqoob, T.; Jiang, P.; Zhou, Y. Y.
Bibcode: 2012ApJ...744L..21S
Altcode: 2011arXiv1112.1569S
  Using Chandra high-energy grating (HEG) observations of 32 active
  galactic nuclei (AGNs), we present a systematic study of the X-ray
  Baldwin effect (XBE; i.e., the anti-correlation between the narrow
  Fe Kα line equivalent width (EW) and X-ray continuum luminosity
  for AGN samples) with the highest spectral resolution currently
  available. We have previously reported an anti-correlation with
  EWvpropL <SUP>-0.22</SUP> <SUB>2-10 keV</SUB> in an HEG sample, and
  the correlation is much weaker after averaging multiple observations of
  individual AGNs (EWvpropL <SUP>-0.13</SUP> <SUB>2-10 keV</SUB>). This
  indicates that rapid variation in the X-ray continuum plays an important
  role in producing the XBE, and such an effect should also be visible
  in individual AGNs. In this Letter, by normalizing the line EWs and
  continuum luminosities to the time-averaged values for each AGN in our
  sample with multiple HEG observations, we find a strong anti-correlation
  between EW and L<SUB>X</SUB> (EW/langEWrangvprop(L/langLrang)<SUP>-0.82
  ± 0.10</SUP>), consistent with the XBE expected in an individual
  AGN if the narrow line flux remains constant while the continuum
  varies. This is first observational evidence that the Fe Kα line
  flux in a large sample of AGNs lacks a corresponding response to
  the continuum variation, supporting the fact that the narrow Fe-K
  line emission originates from a region far from the nucleus. We then
  performed Monte Carlo simulations to address whether the global XBE can
  be produced by X-ray continuum variation solely, and found that such
  an interpretation of the XBE cannot be ruled out statistically. One
  should thus be very cautious before drawing any scientific conclusion
  based on an observed XBE.

Title: The Latitude Distribution of Small-scale Magnetic Elements
    in Solar Cycle 23
Authors: Jin, C. L.; Wang, J. X.
Bibcode: 2012ApJ...745...39J
Altcode:
  With the unique data set from full-disk observations provided by
  Michelson Doppler Imager on board the Solar and Heliospheric Observatory
  in the interval embodying solar cycle 23, we have found that the
  cyclic variations of numbers and total flux of these small-scale
  magnetic elements covering fluxes of (2.9-32.0) × 10<SUP>18</SUP>
  Mx and (4.27-38.01) × 10<SUP>19</SUP> Mx show anticorrelation
  and correlation with sunspots, respectively. In this study, the
  time-latitude distributions of these anticorrelated and correlated
  elements are analyzed. The following results are disclosed: (1)
  for the correlated elements, the cyclic variations of the total flux
  in low-latitude and middle-latitude regions show a longer duration
  of cyclic maximum phase than that of an active region (AR) in the
  corresponding latitude region; the total flux of these elements shows
  the accordant south-north asymmetry with that of AR; the time-latitude
  distribution of their number displays a similar butterfly diagram
  but with a latitude distribution that is twice as wide as that of
  sunspots. (2) For the anticorrelated elements, the time-latitude
  distribution of number shows a solar cycle variation different from
  the sunspot butterfly diagram; in each latitude, the distribution
  of anticorrelated elements always shows the anticorrelated variation
  with that of sunspots; during solar cycle 23, the average speed of the
  peak latitudinal migration for anticorrelated elements reaches 7.5 deg
  year<SUP>-1</SUP>, almost three times that for sunspots. These results
  seem to imply that the correlated elements are the debris of decayed
  sunspots, and the anticorrelated elements have a different source but
  are affected or modulated by sunspot magnetic field.

Title: Statistical properties of superactive regions during solar
    cycles 19-23
Authors: Chen, A. Q.; Wang, J. X.; Li, J. W.; Feynman, J.; Zhang, J.
Bibcode: 2011A&A...534A..47C
Altcode:
  Context. Each solar activity cycle is characterized by a small number
  of superactive regions (SARs) that produce the most violent of space
  weather events with the greatest disastrous influence on our living
  environment. <BR /> Aims: We aim to re-parameterize the SARs and
  study the latitudinal and longitudinal distributions of SARs. <BR />
  Methods: We select 45 SARs in solar cycles 21-23, according to the
  following four parameters: 1) the maximum area of sunspot group, 2)
  the soft X-ray flare index, 3) the 10.7 cm radio peak flux, and 4)
  the variation in the total solar irradiance. Another 120 SARs given
  by previous studies of solar cycles 19-23 are also included. The
  latitudinal and longitudinal distributions of the 165 SARs in both the
  Carrington frame and the dynamic reference frame during solar cycles
  19-23 are studied statistically. <BR /> Results: Our results indicate
  that these 45 SARs produced 44% of all the X class X-ray flares during
  solar cycles 21-23, and that all the SARs are likely to produce a very
  fast CME. The latitudinal distributions of SARs display the Maunder
  butterfly diagrams and SARs occur preferentially in the maximum period
  of each solar cycle. Northern hemisphere SARs dominated in solar cycles
  19 and 20 and southern hemisphere SARs dominated in solar cycles 21 and
  22. In solar cycle 23, however, SARs occurred about equally in each
  hemisphere. There are two active longitudes in both the northern and
  southern hemispheres, about 160°-200° apart. Applying the improved
  dynamic reference frame to SARs, we find that SARs rotate faster than
  the Carrington rate and there is no significant difference between
  the two hemispheres. The synodic periods are 27.19 days and 27.25
  days for the northern and southern hemispheres, respectively. The
  longitudinal distribution of SARs is significantly non-axisymmetric
  and about 75% SARs occurred near two active longitudes with half
  widths of 45°. <P />Appendix A is available in electronic form at
  <A href="http://www.aanda.org">http://www.aanda.org</A>

Title: Chandra High-energy Grating Observations of the Fe Kα Line
Core in Type II Seyfert Galaxies: A Comparison with Type I Nuclei
Authors: Shu, X. W.; Yaqoob, T.; Wang, J. X.
Bibcode: 2011ApJ...738..147S
Altcode: 2011arXiv1107.0195S
  We present a study of the core of the Fe Kα emission line at ~6.4
  keV in a sample of type II Seyfert galaxies observed by the Chandra
  high-energy grating. The sample consists of 29 observations of 10 unique
  sources. We present measurements of the Fe Kα line parameters with
  the highest spectral resolution currently available. In particular,
  we derive the most robust intrinsic line widths for some of the
  sources in the sample to date. We obtained a weighted mean full
  width at half-maximum (FWHM) of 2000 ± 160 km s<SUP>-1</SUP> for
  8 out of 10 sources (the remaining sources had insufficient signal
  to noise). From a comparison with the optical emission-line widths
  obtained from spectropolarimetric observations, we found that the
  location of Fe Kα line-emitting material is a factor of ~0.7-11 times
  the size of the optical broad-line region. Furthermore, compared to 13
  type I active galactic nuclei (AGNs) for which the best Fe Kα line
  FWHM constraints were obtained, we found no difference in the FWHM
  distribution or the mean FWHM, and this conclusion is independent of
  the central black hole mass. This result suggests that the bulk of the
  Fe Kα line emission may originate from a universal region at the same
  radius with respect to the gravitational radius, ~3 × 10<SUP>4</SUP>
  r<SUB>g</SUB> on average. By examining the correlation between the Fe
  Kα luminosity and the [O IV] line luminosity, we found a marginal
  difference in the Fe Kα line flux between type I and type II AGNs,
  but the spread in the ratio of L <SUB>Fe</SUB> to L <SUB>[O IV]</SUB>
  is about two orders of magnitude. Our results confirm the theoretical
  expectation that the Fe Kα emission-line luminosity cannot trivially
  be used as a proxy of the intrinsic AGN luminosity, unless a detailed
  comparison of the data with proper models is applied.

Title: The Sun's Small-scale Magnetic Elements in Solar Cycle 23
Authors: Jin, C. L.; Wang, J. X.; Song, Q.; Zhao, H.
Bibcode: 2011ApJ...731...37J
Altcode: 2011arXiv1102.3728J
  With the unique database from the Michelson Doppler Imager on board
  the Solar and Heliospheric Observatory in an interval embodying solar
  cycle 23, the cyclic behavior of solar small-scale magnetic elements
  is studied. More than 13 million small-scale magnetic elements are
  selected, and the following results are found. (1) The quiet regions
  dominated the Sun's magnetic flux for about 8 years in the 12.25 year
  duration of cycle 23. They contributed (0.94-1.44) ×10<SUP>23</SUP>
  Mx flux to the Sun from the solar minimum to maximum. The monthly
  average magnetic flux of the quiet regions is 1.12 times that of
  the active regions in the cycle. (2) The ratio of quiet region flux
  to that of the total Sun equally characterizes the course of a solar
  cycle. The 6 month running average flux ratio of the quiet regions was
  larger than 90.0% for 28 continuous months from July 2007 to October
  2009, which very well characterizes the grand solar minima of cycles
  23-24. (3) From the small to the large end of the flux spectrum, the
  variations of numbers and total flux of the network elements show
  no correlation, anti-correlation, and correlation with sunspots,
  respectively. The anti-correlated elements, covering the flux of
  (2.9-32.0)×10<SUP>18</SUP> Mx, occupy 77.2% of the total element
  number and 37.4% of the quiet-Sun flux. These results provide insight
  into the reason for anti-correlations of small-scale magnetic activity
  during the solar cycle.

Title: Small-scale magnetic elements in Solar Cycle 23
Authors: Jin, C. L.; Wang, J. X.; Song, Q.; Zhao, H.
Bibcode: 2011arXiv1102.3485J
Altcode:
  With the unique database from Michelson Doppler Imager aboard the
  Solar and Heliospheric Observatory in an interval embodying solar
  cycle 23, the cyclic behavior of solar small-scale magnetic elements
  is studied. More than 13 million small-scale magnetic elements are
  selected, and the following results are unclosed. (1) The quiet regions
  dominated the Sun\textsf{'}s magnetic flux for about 8 years in the
  12.25 year duration of Cycle 23. They contributed (0.94 -- 1.44) $\times
  10^{23}$ Mx flux to the Sun from the solar minimum to maximum. The
  monthly average magnetic flux of the quiet regions is 1.12 times that of
  active regions in the cycle. (2) The ratio of quiet region flux to that
  of the total Sun equally characterizes the course of a solar cycle. The
  6-month running-average flux ratio of quiet region had been larger than
  90.0% for 28 continuous months from July 2007 to October 2009, which
  characterizes very well the grand solar minima of Cycles 23-24. (3)
  From the small to large end of the flux spectrum, the variations of
  numbers and total flux of the network elements show no-correlation,
  anti-correlation, and correlation with sunspots, respectively. The
  anti-correlated elements, covering the flux of (2.9 - 32.0)$\times
  10^{18}$ Mx, occupies 77.2% of total element number and 37.4% of quiet
  Sun flux. These results provide insight into reason for anti-correlated
  variations of small-scale magnetic activity during the solar cycle.

Title: A current sheet traced from the Sun to interplanetary space
Authors: Zhou, G. P.; Xiao, C. J.; Wang, J. X.; Wheatland, M. S.;
   Zhao, H.
Bibcode: 2011A&A...525A.156Z
Altcode:
  Context. Magnetic reconnection is a central concept for understanding
  solar activity, including filament eruptions, flares, and coronal mass
  ejections (CMEs). The existence of transverse and vertical current
  sheets, sites where reconnection takes place in the solar atmosphere,
  is frequently proposed as a precondition for flare/CME models, but is
  rarely identified in observations. <BR /> Aims: We aim at identifying
  a transverse current sheet that existed in the pre-CME structure and
  persisted from the CME solar source to interplanetary space. <BR />
  Methods: STEREO A/B provide us a unique opportunity to calculate the
  interplanetary current sheets for the magnetic cloud. We analyze
  such a structure related to the fast halo CME of 2006 December 13
  with assembled observations. A current sheet at the front of the
  magnetic cloud is analyzed to its origin in a transverse current
  sheet in the CME solar source, which can be revealed in the magnetic
  field extrapolations, XRT, and LASCO observations. <BR /> Results:
  An interplanetary current sheet is identified as coming from the CME
  solar source by carefully mapping and examining multiple observations
  from the Sun to interplanetary space, along with nonlinear force-free
  magnetic field extrapolations of the active region NOAA 10930. <BR />
  Conclusions: The structure identified in the pre-flare state is a global
  transverse current sheet, which plays a role in the CME initiation,
  and propagates from the corona to interplanetary space.

Title: Solar cycle variation of network magnetic elements
Authors: Wang, J. X.; Jin, C. L.
Bibcode: 2011ASInC...2..163W
Altcode:
  With the unique database from Michelson Doppler Imager aboard the
  Solar and Heliospheric Observatory in an interval embodying solar
  cycle 23, the cyclic behavior of solar small-scale magnetic elements
  is studied. More than 13 million solar network magnetic elements are
  selected, and the following results are discussed. (1) With increasing
  flux per element, the number variation of the network elements shows a
  three-fold scenario: no-correlation, anti-correlation, and correlation
  with sunspots, respectively. The anti-correlated elements cover
  flux range of (2.9 - 32.0)× 10^{18} Mx, and occupy 77.2% of total
  network elements. (2) The latitude distribution of the correlated
  elements follows the sunspot butterfly diagram in the solar cycle
  but has wider latitude distribution than sunspots. Furthermore, the
  anti-correlated elements also show much broad latitude distribution,
  but a moderate migration toward equator during the solar maximum which
  was clearly out of phase with sunspots. These results shed new light
  in understanding anti-correlated variations of small-scale solar
  activity, e.g., X-ray coronal bright points, and the origin of the
  Sun's small-scale magnetism.

Title: Erratum to: Solar Intranetwork Magnetic Elements: Evolution
    and Lifetime
Authors: Zhou, G. P.; Wang, J. X.; Jin, C. L.
Bibcode: 2010SoPh..267..493Z
Altcode: 2010SoPh..tmp..221Z; 2010SoPh..tmp..197Z
  No abstract at ADS

Title: Solar Intranetwork Magnetic Elements: Evolution and Lifetime
Authors: Zhou, G. P.; Wang, J. X.; Jin, C. L.
Bibcode: 2010SoPh..267...63Z
Altcode: 2010SoPh..tmp..173Z
  Based on Hinode SOT/NFI observations with greatly improved spatial
  and temporal resolution and polarization sensitivity, the lifestory
  of the intranetwork (IN) magnetic elements are explored in a solar
  quiet region. A total of 2282 IN elements are followed from their
  appearance to disappearance and their fluxes measured. By tracing
  individual IN elements their lifetimes are obtained, which fall in
  the range from 1 to 20 min. The average lifetime is 2.9±2.0 min. The
  observed lifetime distribution is well represented by an exponential
  function. Therefore, the e-fold characteristic lifetime is determined by
  a least-square fitting to the observations, which is 2.1±0.3 min. The
  lifetime of IN elements is correlated closely with their flux. The
  evolution of IN elements is described according to the forms of their
  birth and disappearance. Based on the lifetime and flux obtained from
  the new observations, it is estimated that the IN elements have the
  capacity of heating the corona with a power of 2.1×10<SUP>28</SUP>
  erg s<SUP>−1</SUP> for the whole Sun.

Title: XMM-Newton Observations of the Seyfert 2 Galaxy NGC 7590:
    The Nature of X-ray Absorption
Authors: Shu, X. W.; Liu, T.; Wang, J. X.
Bibcode: 2010ApJ...722...96S
Altcode: 2010arXiv1008.1502S
  We present the analysis of three XMM-Newton observations of the Seyfert
  2 galaxy NGC 7590. The source was found to have no X-ray absorption
  in the low spatial resolution ASCA data. The XMM-Newton observations
  provide a factor of ~10 better spatial resolution than previous ASCA
  data. We find that the X-ray emission of NGC 7590 is dominated by an
  off-nuclear ultra-luminous X-ray source and an extended emission from
  the host galaxy. The nuclear X-ray emission is rather weak compared
  with the host galaxy. Based on its very low X-ray luminosity as well
  as the small ratio between the 2-10 keV and the [O III] fluxes, we
  interpret NGC 7590 as Compton-thick rather than being an "unobscured"
  Seyfert 2 galaxy. Future higher resolution observations such as Chandra
  are crucial to shed light on the nature of the NGC 7590 nucleus.

Title: X-ray Properties of the z ~ 4.5 Lyα Emitters in the Chandra
    Deep Field South Region
Authors: Zheng, Z. Y.; Wang, J. X.; Finkelstein, S. L.; Malhotra,
   S.; Rhoads, J. E.; Finkelstein, K. D.
Bibcode: 2010ApJ...718...52Z
Altcode: 2010arXiv1005.3829Z
  We report the first X-ray detection of Lyα emitters (LAEs) at
  redshift z ~ 4.5. One source (J033127.2-274247) is detected in the
  Extended Chandra Deep Field-South (ECDF-S) X-ray data and has been
  spectroscopically confirmed as a z = 4.48 quasar with L<SUB>X</SUB> =
  4.2 × 10<SUP>44</SUP> erg s<SUP>-1</SUP>. The single detection gives
  an Lyα quasar density of ~ 2.7<SUP>+6.2</SUP> <SUB>-2.2</SUB> ×
  10<SUP>-6</SUP> Mpc<SUP>-3</SUP>, consistent with the X-ray luminosity
  function of quasars. Another 22 LAEs in the central Chandra Deep
  Field-South region are not detected individually, but their co-added
  counts yield an S/N = 2.4 (p = 99.83%) detection at soft band, with an
  effective exposure time of ~36 Ms. Further analysis of the equivalent
  width (EW) distribution shows that all the signals come from 12 LAE
  candidates with EW<SUB>rest</SUB>&lt; 400 Å and 2 of them contribute
  about half of the signal. From follow-up spectroscopic observations,
  we find that one of the two is a low-redshift emission-line galaxy,
  and the other is a Lyman break galaxy at z = 4.4 with little or no Lyα
  emission. Excluding these two and combined with ECDF-S data, we derive a
  3σ upper limit on the average X-ray flux of F <SUB>0.5-2.0 keV</SUB>
  &lt; 1.6 × 10<SUP>-18</SUP> erg cm<SUP>-2</SUP> s<SUP>-1</SUP>,
  which corresponds to an average luminosity of langL <SUB>0.5-2
  keV</SUB>rang &lt;2.4 × 10<SUP>42</SUP> erg s<SUP>-1</SUP> for z ~
  4.5 LAEs. If the average X-ray emission is due to star formation,
  it corresponds to a star formation rate (SFR) of &lt;180-530 M
  <SUB>sun</SUB> yr<SUP>-1</SUP>. We use this SFR<SUB> X </SUB> as an
  upper limit of the unobscured SFR to constrain the escape fraction
  of Lyα photons and find a lower limit of f <SUB>esc,Lyα</SUB> &gt;
  3%-10%. However, our upper limit on the SFR<SUB> X </SUB> is ~7 times
  larger than the upper limit on SFR<SUB> X </SUB> on z ~ 3.1 LAEs in
  the same field and at least 30 times higher than the SFR estimated from
  Lyα emission. From the average X-ray-to-Lyα line ratio, we estimate
  that fewer than 3.2% (6.3%) of our LAEs could be high-redshift type 1
  (type 2) active galactic nuclei (AGNs) and those hidden AGNs likely
  show low rest-frame EWs.

Title: The Cores of the Fe Kα Lines in Active Galactic Nuclei:
    An Extended Chandra High Energy Grating Sample
Authors: Shu, X. W.; Yaqoob, T.; Wang, J. X.
Bibcode: 2010ApJS..187..581S
Altcode: 2010arXiv1003.1790S
  We extend the study of the core of the Fe Kα emission line at ~6.4
  keV in Seyfert galaxies reported by Yaqoob &amp; Padmanabhan using a
  larger sample observed by the Chandra high-energy grating (HEG). The
  sample consists of 82 observations of 36 unique sources with z &lt;
  0.3. Whilst heavily obscured active galactic nuclei are excluded
  from the sample, these data offer some of the highest precision
  measurements of the peak energy of the Fe Kα line, and the highest
  spectral resolution measurements of the width of the core of the line in
  unobscured and moderately obscured (N <SUB>H</SUB> &lt; 10<SUP>23</SUP>
  cm<SUP>-2</SUP>) Seyfert galaxies to date. From an empirical and uniform
  analysis, we present measurements of the Fe Kα line centroid energy,
  flux, equivalent width (EW), and intrinsic width (FWHM). The Fe Kα line
  is detected in 33 sources, and its centroid energy is constrained in
  32 sources. In 27 sources, the statistical quality of the data is good
  enough to yield measurements of the FWHM. We find that the distribution
  in the line centroid energy is strongly peaked around the value for
  neutral Fe, with over 80% of the observations giving values in the
  range 6.38-6.43 keV. Including statistical errors, 30 out of 32 sources
  (~94%) have a line centroid energy in the range 6.35-6.47 keV. The mean
  EW, among the observations in which a non-zero lower limit could be
  measured, was 53 ± 3 eV. The mean FWHM from the subsample of 27 sources
  was 2060 ± 230 km s<SUP>-1</SUP>. The mean EW and FWHM are somewhat
  higher when multiple observations for a given source are averaged. From
  a comparison with the Hβ optical emission-line widths (or, for one
  source, Brα), we find that there is no universal location of the Fe
  Kα line-emitting region relative to the optical broad-line region
  (BLR). In general, a given source may have contributions to the Fe Kα
  line flux from parsec-scale distances from the putative black hole, down
  to matter a factor ~2 closer to the black hole than the BLR. We confirm
  the presence of the X-ray Baldwin effect, an anti-correlation between
  the Fe Kα line EW and X-ray continuum luminosity. The HEG data have
  enabled isolation of this effect to the narrow core of the Fe Kα line.

Title: NGC 2992 in an X-ray High State Observed by XMM-Newton:
    Response of the Relativistic Fe Kα Line to the Continuum
Authors: Shu, X. W.; Yaqoob, T.; Murphy, K. D.; Braito, V.; Wang,
   J. X.; Zheng, W.
Bibcode: 2010ApJ...713.1256S
Altcode: 2010arXiv1003.1789S
  We present the analysis of an XMM-Newton observation of the Seyfert
  galaxy NGC 2992. The source was found in its highest level of X-ray
  activity yet detected, a factor ~23.5 higher in the 2-10 keV flux
  than the historical minimum. NGC 2992 is known to exhibit X-ray
  flaring activity on timescales of days to weeks, and the XMM-Newton
  data provide at least a factor of ~3 better spectral resolution in
  the Fe K band than any previously measured flaring X-ray state. We
  find that there is a broad feature in the ~5-7 keV band that could be
  interpreted as a relativistic Fe Kα emission line. Its flux appears
  to have increased in tandem with the 2-10 keV continuum when compared
  to a previous Suzaku observation when the continuum was a factor of
  ~8 lower than that during the XMM-Newton observation. The XMM-Newton
  data are consistent with the general picture that increased X-ray
  activity and corresponding changes in the Fe Kα line emission occur
  in the innermost regions of the putative accretion disk. This behavior
  contrasts with the behavior of other active galactic nuclei in which
  the Fe Kα line does not respond to variability in the X-ray.

Title: Is there more global solar activity on the Sun?
Authors: Wang, J. X.; Zhang, Y. Z.; Zhou, G. P.; Wen, Y. Y.; Jiang, J.
Bibcode: 2010IAUS..264..251W
Altcode:
  There appear indications of more global activity on the Sun
  which is larger, much beyond the scale of solar active regions
  (ARs). These indications include formation, flaring and eruption of the
  trans-equatorial loops seen in EUV and X-rays, formation and eruption of
  trans-equatorial filaments, global magnetic connectivity in EUV dimming
  associated with halo-coronal mass ejections, wide spread of radio burst
  sources in meter wavelength in the solar corona, and quasi-simultaneous
  magnetic flux emergence in both hemispheres seen during some major solar
  events. With examples of a few major events in the last solar cycle we
  discuss the possibility that there is large or global-scale activity
  on the Sun. Its spatial scale is many times larger than that of AR
  and temporal scale is over 10 hours. The exemplified trans-equatorial
  loops are anchored in ARs and their activity is temporally associated
  with flares in ARs too. In some sense the flares in ARs appear either
  as a part of or a precursor of the more global activity. It is likely
  that the combination of the flares in ARs and the associated global
  activity is responsible to the major solar-terrestrial events. More
  efforts in understanding the global activity are undertaken.

Title: The Research on the Fast Static Precise Point Position Based
    on Ridged Estimation
Authors: Li, H. J.; Wang, J. X.; Chen, J. P.; Hu, C. W.
Bibcode: 2009AcASn..50..438L
Altcode:
  Precise Point Positioning (PPP) has been reported to have a precision at
  centimeter level in static mode and at centimeter to decimeter level in
  kinematic mode. However, the application of PPP to real-time is still
  limited by its long convergence time, typically 30 minutes, which
  is necessary for the float carrier phase ambiguity resolution. The
  ambiguity free model of PPP can eliminate the initial phase
  ambiguities through epoch-difference of phase observations. However,
  this mode only estimates coordinate differences between two sequential
  epochs. Therefore, the station coordinates need to be derived with
  additional methods, e.g., combined with noised range observations. In
  this paper, based on the phase epoch-difference, a fast static PPP
  algorithm is developed, where parameters estimation is based on the
  ridged estimation. The coordinates can be estimated by observations
  only at two epochs, assuring the fast PPP. Using the 1 hour-data
  collected on the 295th day of 2007 in Tongji University, a test was
  carried out. Results show that the coordinate precision can be at
  centimeter to decimeter level when the initial values are different.

Title: Magnetic non-potentiality on the quiet Sun and the filigree
Authors: Zhao, Meng; Wang, Jing-Xiu; Jin, Chun-Lan; Zhou, Gui-Ping
Bibcode: 2009RAA.....9..933Z
Altcode:
  From the observed vector magnetic fields by the Solar Optical
  Telescope/Spectro-Polarimeter aboard the satellite Hinode, we have
  examined whether or not the quiet Sun magnetic fields are non-potential,
  and how the G-band filigrees and Ca II network bright points (NBPs)
  are associated with the magnetic non-potentiality. A sizable
  quiet region in the disk center is selected for this study. The
  new findings by the study are as follows. (1) The magnetic fields
  of the quiet region are obviously non-potential. The region-average
  shear angle is 40<SUP>o</SUP>, the average vertical current is 0.016A
  m<SUP>-2</SUP>, and the average free magnetic energy density, 2.7 ×
  10<SUP>2</SUP> erg cm<SUP>-3</SUP>. The magnitude of these non-potential
  quantities is comparable to that in solar active regions. (2) There
  are overall correlations among current helicity, free magnetic
  energy and longitudinal fields. The magnetic non-potentiality is
  mostly concentrated in the close vicinity of network elements which
  have stronger longitudinal fields. (3) The filigrees and NBPs are
  magnetically characterized by strong longitudinal fields, large electric
  helicity, and high free energy density. Because the selected region
  is away from any enhanced network, these new results can generally
  be applied to the quiet Sun. The findings imply that stronger network
  elements play a role in high magnetic non-potentiality in heating the
  solar atmosphere and in conducting the solar wind.

Title: Flare-induced signals in polarization measurements during
    the X2.6 flare on 2005 January 15
Authors: Zhao, Meng; Wang, Jing-Xiu; Matthews, Sarah; Ming-DeDing;
   Zhao, Hui; Jin, Chun-Lan
Bibcode: 2009RAA.....9..812Z
Altcode:
  Flare-induced signals in polarization measurements which were manifested
  as apparent polarity reversal in magnetograms have been reported since
  1981. We are motivated to further quantify the phenomenon by asking
  two questions: can we distinguish the flare-induced signals from real
  magnetic changes during flares, and what we can learn about flare
  energy release from the flare-induced signals? We select the X2.6 flare
  that occurred on 2005 January 15, for further study. The flare took
  place in NOAA active region (AR) 10720 at approximately the central
  meridian, which makes the interpretation of the vector magnetograms
  less ambiguous. We have identified that flare-induced signals during
  this flare appeared in six zones. The zones are located within an
  average distance of 5 Mm from their weight center to the main magnetic
  neutral line, have an average size of (0.6±0.4)×10<SUP>17</SUP>
  cm<SUP>2</SUP>, duration of 13±4 min, and flux density change of
  181±125 G in the area of reversed polarity. The following new facts
  have been revealed by this study: (1) the flare-induced signal is
  also seen in the transverse magnetograms but with smaller magnitude,
  e.g., about 50 G; (2) the flare-induced signal mainly manifests itself
  as apparent polarity reversal, but the signal starts and ends as a
  weakening of flux density; (3) The flare-induced signals appear in
  phase with the peaks of hard X-ray emission as observed by the Ramaty
  High Energy Solar Spectroscopic Imager (RHESSI), and mostly trace the
  position of RHESSI hard X-ray footpoint sources. (4) in four zones,
  it takes place co-temporally with real magnetic changes which persist
  after the flare. Only for the other two zones does the flux density
  recover to the pre-flare level immediately after the flare. The physical
  implications of the flare-induced signal are discussed in view of its
  relevance to the non-thermal electron precipitation and primary energy
  release in the flare.

Title: Magnetic interactions during sympathetic solar eruptions
Authors: Jiang, Yun-Chun; Bi, Yi; Yang, Jia-Yan; Zheng, Rui-Sheng;
   Wang, Jing-Xiu
Bibcode: 2009RAA.....9..603J
Altcode:
  We present the first evidence for occurrences of magnetic interactions
  between a jet, a filament and coronal loops during a complex event,
  in which two flares sequentially occurred at different positions of
  the same active region and were closely associated with two successive
  coronal mass ejections (CMEs), respectively. The coronal loops were
  located outside but nearby the filament channel before the flares. The
  jet, originating from the first flare during its rise phase, not only
  hit the filament body but also met one of the ends of the loops. The
  filament then underwent an inclined eruption followed by the second
  flare and met the same loop end once more. Both the jet and the filament
  eruption were accompanied by the development of loop disturbances and
  the appearances of brightenings around the meeting site. In particular,
  the erupting filament showed clear manifestations of interactions with
  the loops. After a short holdup, only its portion passed through this
  site, while the other portion remained at the same place. Following
  the filament eruption and the loop disappearance, four dimmings were
  formed and located near their four ends. This is a situation that we
  define as “quadrupolar dimmings." It appears that the two flares
  consisted of a sympathetic pair physically linked by the interaction
  between the jet and the filament, and their sympathy indicated that
  of the two CMEs. Moreover, it is very likely that the two sympathetic
  CMEs were simultaneously associated with the disappearing loops and
  the quadrupole dimmings.

Title: On VI Emission in Nuclear Region of NGC 1068
Authors: Zheng, W.; Kriss, G. A.; Wang, J. -X.; Sahnow, D.; Allen,
   M.; Dopita, M.; Tsvetanov, Z.; Bicknell, G.
Bibcode: 2009AIPC.1135...52Z
Altcode:
  FUSE Spectra of the nuclear region of NGC 1068 find strong OVI
  emission consisting of a pair of narrow and broad components. There
  is a gradient in the velocity field for the narrow O VI component
  of ~200 kms<SUP>-1</SUP> from ~2'' southwest of the nucleus to ~4''
  northeast. A similar pattern is also observed with the broad O VI
  component, with a gradient of ~3000 kms<SUP>-1</SUP>. These results
  are consistent with the HST/STIS findings and suggest a biconical
  structure in which the velocity field is mainly radial outflow.

Title: The application of the LAMBDA method in the estimation of
    the GPS slant wet vapour
Authors: Huang, S. Q.; Wang, J. X.; Wang, X. Y.; Chen, J. P.
Bibcode: 2009AcASn..50...60H
Altcode:
  By far, the technology of GPS data processing has been improved well
  and the accuracy of this processing has increased greatly. So, GPS has
  been applied in meteorology widely.The SWV (Slant Wet Vapour) is a very
  important parameter in the GPS meteorology. In 2004, Song Shuli had
  advanced a SWV estimation method which used the precision orbit of JPL,
  IGS clock and the LC observations without cycle-slip. But this method
  is bad in real-time character. LAMBDA method, which is working well in
  the VRS (Virtual Reference Station) /COORS, is used in the ambiguity
  estimation. The method was proved by some true data calculation. The
  ZTD(Zenith Time Delay), which is calculated by projecting SWD (Slant
  Wet Delay) to zenith direction, has good coherence. Compairing the
  ZTD with the results of GAMIT and BERNESE, the deviation between our
  result and the GAMIT one is commonly little than 3cm, and the BERNESE
  one is commonly little than 1.5cm.

Title: Commission 10: Solar Activity
Authors: Klimchuk, James A.; van Driel-Gesztelyi, Lidia; Schrijver,
   Carolus J.; Melrose, Donald B.; Fletcher, Lyndsay; Gopalswamy,
   Natchimuthuk; Harrison, Richard A.; Mandrini, Cristina H.; Peter,
   Hardi; Tsuneta, Saku; Vršnak, Bojan; Wang, Jing-Xiu
Bibcode: 2009IAUTA..27...79K
Altcode: 2008arXiv0809.1444K
  Commission 10 deals with solar activity in all of its forms,
  ranging from the smallest nanoflares to the largest coronal mass
  ejections. This report reviews scientific progress over the roughly
  two-year period ending in the middle of 2008. This has been an exciting
  time in solar physics, highlighted by the launches of the Hinode and
  STEREO missions late in 2006. The report is reasonably comprehensive,
  though it is far from exhaustive. Limited space prevents the inclusion
  of many significant results. The report is divided into the following
  sections: Photosphere and chromosphere; Transition region; Corona and
  coronal heating; Coronal jets; flares; Coronal mass ejection initiation;
  Global coronal waves and shocks; Coronal dimming; The link between low
  coronal CME signatures and magnetic clouds; Coronal mass ejections in
  the heliosphere; and Coronal mass ejections and space weather. Primary
  authorship is indicated at the beginning of each section.

Title: Relativistic Outflows in Two Quasars in the Chandra Deep
    Field South
Authors: Zheng, Z. Y.; Wang, J. X.
Bibcode: 2008ApJ...688..116Z
Altcode: 2008arXiv0807.4669Z
  In this paper we provide new 1 Ms Chandra ACIS spectra of two quasars
  in the Chandra Deep Field South (CDF-S) which had strong and extremely
  blueshifted X-ray emission/absorption line features in previous 1 Ms
  spectra, with outflowing bulk velocity v ~ 0.65-0.84c. In the new 1 Ms
  spectra, the relativistic blueshifted line feature is solidly confirmed
  in CXO CDFS J033225.3-274219 (CDFS 46, z = 1.617), and marginally
  visible in CXO CDFS J033260.0-274748 (CDFS 11, z = 2.579), probably due
  to the increased Chandra ACIS background in the new 1 Ms exposure. The
  new data rule out the possibility (although very tiny already based
  on the old 1Ms data) that the two sources were selected to be unusual
  due to noise spikes in the spectra. The only likely interpretation is
  extremely blueshifted iron absorption/emission lines or an absorption
  edge due to relativistic outflow. We find that the rest-frame emission
  line center in CDFS 46 marginally decreased from 16.2 to 15.2 keV after
  7 years. The line shift could be due to either a decreasing outflowing
  velocity or a lower ionization level. Including the two quasars reported
  in this paper, we collect a total of 7 quasars from the literature
  showing blueshifted emission or absorption line features with v &gt;=
  0.4c in X-ray spectra, and discuss their connection to jet and/or BAL
  (broad absorption line) outflows.

Title: A magnetic null geometry reconstructed from Cluster spacecraft
    observations
Authors: He, J. -S.; Tu, C. -Y.; Tian, H.; Xiao, C. -J.; Wang, X. -G.;
   Pu, Z. -Y.; Ma, Z. -W.; Dunlop, M. W.; Zhao, H.; Zhou, G. -P.; Wang,
   J. -X.; Fu, S. -Y.; Liu, Z. -X.; Zong, Q. -G.; Glassmeier, K. -H.;
   Reme, H.; Dandouras, I.; Escoubet, C. P.
Bibcode: 2008JGRA..113.5205H
Altcode:
  This paper reports for the first time the identification of a magnetic
  structure around a magnetic null in a magnetic reconnection region
  in the magnetotail. Magnetic reconnection is one of the fundamental
  processes in astrophysical and solar-terrestrial plasmas. Though
  the concept of reconnection has been studied for many years,
  the process that really occurs has not been fully revealed by
  direct measurements. In particular, the lack of a description of
  three-dimensional (3-D) reconnecting magnetic field from observations
  makes the task more difficult. The Cluster spacecraft array provide an
  opportunity to reconstruct the 3-D magnetic reconnection structure based
  on magnetic field vectors simultaneously measured at four positions. The
  identification of this structure comes from a new method of analysis
  of in situ measurements proposed here. Applying a fitting model of 10
  spherical harmonic functions and a Harris current sheet function, plus
  a constant field, we reconstruct a 3-D magnetic field configuration
  around the magnetic null in an reconnection event observed by Cluster
  in the geo-magnetotail.

Title: Determination of the Topology Skeleton of Magnetic Fields in
    a Solar Active Region
Authors: Zhao, Hui; Wang, Jing-Xiu; Zhang, Jun; Xiao, Chi-Jie;
   Wang, Hai-Min
Bibcode: 2008ChJAA...8..133Z
Altcode: 2007arXiv0712.3319Z
  Magnetic topology has been a key to the understanding of magnetic
  energy release mechanism. Based on observed vector magnetograms, we
  have determined the three-dimensional (3D) topology skeleton of the
  magnetic fields in the active region NOAA 10720. The skeleton consists
  of six 3D magnetic nulls and a network of corresponding spines, fans,
  and null-null lines. For the first time, we have identified a spiral
  magnetic null in Sun's corona. The magnetic lines of force twisted
  around the spine of the null, forming a `magnetic wreath' with excess
  of free magnetic energy and resembling observed brightening structures
  at extra-ultraviolet (EUV) wavebands. We found clear evidence of
  topology eruptions which are referred to as catastrophic changes of
  topology skeleton associated with a coronal mass ejection (CME) and an
  explosive X-ray flare. These results shed new lights on the structural
  complexity and its role in explosive magnetic activity. The concept of
  flux rope has been widely used in modelling explosive magnetic activity,
  although their observational identity is rather obscure or, at least,
  lacking of necessary details up to date. We suggest that the magnetic
  wreath associated with the 3D spiral null is likely an important class
  of the physical entity of flux ropes.

Title: Chandra X-Ray Sources in the LALA Cetus Field
Authors: Wang, J. X.; Zheng, Z. Y.; Malhotra, S.; Finkelstein, S. L.;
   Rhoads, J. E.; Norman, C. A.; Heckman, T. M.
Bibcode: 2007ApJ...669..765W
Altcode: 2007arXiv0707.3239W
  The 174 ks Chandra Advanced CCD Imaging Spectrometer exposure of
  the Large Area Lyman Alpha Survey (LALA) Cetus field is the second
  of the two deep Chandra images on LALA fields. In this paper we
  present the Chandra X-ray sources detected in the Cetus field, along
  with an analysis of X-ray source counts, stacked X-ray spectrum, and
  optical identifications. A total of 188 X-ray sources were detected:
  174 in the 0.5-7.0 keV band, 154 in the 0.5-2.0 keV band, and 113
  in the 2.0-7.0 keV band. The X-ray source counts were derived and
  compared with LALA field (172 ks exposure). Interestingly, we find
  consistent hard-band X-ray source density, but (36+/-12)% higher
  soft-band X-ray source density in Cetus field. The weighted stacked
  spectrum of the detected X-ray sources can be fitted by a power law
  with photon index Γ=1.55. Based on the weighted stacked spectrum,
  we find that the resolved fraction of the X-ray background drops from
  (72+/-1)% at 0.5-1.0 keV to (63+/-4)% at 6.0-8.0 keV. The unresolved
  spectrum can be fitted by a power law over the range 0.5-7 keV, with a
  photon index Γ=1.22. We also present optical counterparts for 154 of
  the X-ray sources, down to a limiting magnitude of r<SUP>'</SUP>=25.9
  (Vega), using a deep r'-band image obtained with the MMT. <P />Optical
  Observations reported here were obtained at the MMT Observatory, a joint
  facility of the University of Arizona and the Smithsonian Institution.

Title: Nuclear Obscuration in Seyfert 2 Galaxies with and without
    Polarized Broad Emission Lines
Authors: Shu, X. W.; Wang, J. -X.; Jang, P.; Fan, L. L.; Wang, T. -G.
Bibcode: 2007ASPC..373..507S
Altcode:
  We compiled a sample of 54 Seyfert 2 galaxies with both
  spectropolarimetric and X-ray observations to investigate the role
  of nuclear obscuration in the visibility of polarized broad emission
  lines (PBL). We find that at L<SUB>[O III]</SUB> &gt; 10<SUP>41</SUP>
  ergs s<SUP>-1</SUP>, Seyfert 2 galaxies without PBL are more obscured
  in X-ray (at a confidence level of 99%). Our results explain the
  non-detections of PBL under the framework of the unified model, and
  put strong constraint on the geometry of the obscuring torus and the
  scattering region.

Title: On the X-ray Baldwin Effect for the Narrow Fe Kα Emission Line
Authors: Jiang, P.; Wang, J. -X.; Wang, T. -G.
Bibcode: 2007ASPC..373..143J
Altcode:
  We build a large AGN sample with narrow FeK line measurements by
  combining the archival Chandra HETG observations of 34 type 1 AGNs with
  XMM-Newton observations in literature. We find a similar X-ray Baldwin
  effect as reported earlier by Page et al. in the sample; however,
  we note that the anti-correlation is dominated by the radio-loud
  AGN in the sample, whose X-ray spectra might be contaminated by the
  relativistic jet. Excluding the radio-loud AGN, we find a much weaker
  anti-correlation. We present Monte Carlo simulations showing that such
  a weak anti-correlation can be attributed to the relative short time
  scale variations of the X-ray continuum.

Title: Polarization of Quasars: Rotated and Funnel-shaped Outflow
Authors: Wang, H. -Y.; Wang, T. -G.; Wang, J. -X.
Bibcode: 2007ASPC..373..335W
Altcode: 2006astro.ph.12339W
  Polarization is a useful probe to investigate the geometries and
  dynamics of outflows in BAL QSOs. We perform a Monte Carlo simulation to
  calculate the polarization produced by resonant and electron scattering
  in BALR. We find: 1) A rotated and funnel-shaped outflow is preferred
  to explain many observed polarization features. 2) Resonant scattering
  can contribute a significant part of the N V emission line in some QSOs.

Title: Satellite observations of separator-line geometry of
    three-dimensional magnetic reconnection
Authors: Xiao, C. J.; Wang, X. G.; Pu, Z. Y.; Ma, Z. W.; Zhao, H.;
   Zhou, G. P.; Wang, J. X.; Kivelson, M. G.; Fu, S. Y.; Liu, Z. X.;
   Zong, Q. G.; Dunlop, M. W.; Glassmeier, K. -H.; Lucek, E.; Reme, H.;
   Dandouras, I.; Escoubet, C. P.
Bibcode: 2007NatPh...3..609X
Altcode: 2007arXiv0705.1021X
  Detection of a separator line that connects magnetic nulls and
  the determination of the dynamics and plasma environment of such a
  structure can improve our understanding of the three-dimensional (3D)
  magnetic reconnection process. However, this type of field and particle
  configuration has not been directly observed in space plasmas. Here we
  report the identification of a pair of nulls, the null-null line that
  connects them, and associated fans and spines in the magnetotail of
  the Earth using data from the four Cluster spacecraft. With di and de
  designating the ion and electron inertial lengths, respectively, the
  separation between the nulls is found to be ~0.7+/-0.3d<SUB>i</SUB>
  and an associated oscillation is identified as a lower-hybrid wave
  with wavelength ~d<SUB>e</SUB>. This in situ evidence of the full 3D
  reconnection geometry and associated dynamics provides an important
  step towards establishing an observational framework of 3D reconnection.

Title: A Catastrophic Flux Rope in a Quadrupole Magnetic Field for
    Coronal Mass Ejections
Authors: Zhang, Y. -Z.; Wang, J. -X.
Bibcode: 2007ApJ...663..592Z
Altcode:
  We propose a flux-rope model for the initiation of flare-associated
  CMEs. The model triggers the eruption with a catastrophic loss of MHD
  equilibrium and then requires magnetic reconnection to sustain the
  eruption's acceleration. We carry out 2.5-dimensional time-dependent
  resistive MHD simulations, choosing the initial state such that a flux
  rope embedded in a quadrupole field is attached to the solar surface;
  we then increase the magnetic flux of the rope by two different amounts,
  thus obtaining two cases. One exhibits a gradual acceleration of the
  flux rope, whereas the other produces an immediate acceleration. In
  both cases, the maximum speed of the flux rope is representative of
  a fast CME. Thus, we conclude that the flux-rope dynamics depends on
  the intensity of the emergent magnetic flux. Our model does reproduce
  the three-component structure of CMEs.

Title: A Study of the Periodicities of Solar Filament Activity
Authors: Song, Wen-bin; Wang, Jing-xiu
Bibcode: 2007ChA&A..31..270S
Altcode:
  Using the filament catalogues of Meudon Observatory, France, we
  have compiled a daily count sequence of filaments from July 1957
  to December 2004 and carried out a periodicity analysis with the
  Scargle periodogram and Morlet wavelet transform. It is discovered
  that this sequence exhibits four evident periods: 1557, 1141, 795 and
  367 days. The characteristics of the variations of these periods are
  analyzed in detail and the phases, physical mechanisms as well as the
  mutual relations of some of the periods are briefly discussed.

Title: A dynamo model for axisymmetric and non-axisymmetric solar
    magnetic fields
Authors: Jiang, J.; Wang, J. X.
Bibcode: 2007MNRAS.377..711J
Altcode: 2007astro.ph..2508J; 2007MNRAS.tmp..253J
  More and more observations are showing a relatively weak, but
  persistent, non-axisymmetric magnetic field co-existing with the
  dominant axisymmetric field on the Sun. Its existence indicates that the
  non-axisymmetric magnetic field plays an important role in the origin
  of solar activity. A linear non-axisymmetric α<SUP>2</SUP>-Ω dynamo
  model is derived to explore the characteristics of the axisymmetric
  (m = 0) and the first non-axisymmetric (m = 1) modes and to provide
  a theoretical basis with which to explain the `active longitude',
  `flip-flop' and other non-axisymmetric phenomena. The model consists of
  an updated solar internal differential rotation, a turbulent diffusivity
  varying with depth, and an α-effect working at the tachocline in a
  rotating spherical system. The difference between the α<SUP>2</SUP>-Ω
  and the α-Ω models and the conditions that favour the non-axisymmetric
  modes under solar-like parameters are also presented.

Title: Determination of the ν<SUB>e</SUB> and total B8 solar neutrino
    fluxes using the Sudbury Neutrino Observatory Phase I data set
Authors: Aharmim, B.; Ahmad, Q. R.; Ahmed, S. N.; Allen, R. C.;
   Andersen, T. C.; Anglin, J. D.; Bühler, G.; Barton, J. C.; Beier,
   E. W.; Bercovitch, M.; Bergevin, M.; Bigu, J.; Biller, S. D.; Black,
   R. A.; Blevis, I.; Boardman, R. J.; Boger, J.; Bonvin, E.; Boulay,
   M. G.; Bowler, M. G.; Bowles, T. J.; Brice, S. J.; Browne, M. C.;
   Bullard, T. V.; Burritt, T. H.; Cameron, J.; Chan, Y. D.; Chen, H. H.;
   Chen, M.; Chen, X.; Cleveland, B. T.; Cowan, J. H. M.; Cowen, D. F.;
   Cox, G. A.; Currat, C. A.; Dai, X.; Dalnoki-Veress, F.; Davidson,
   W. F.; Deng, H.; Dimarco, M.; Doe, P. J.; Doucas, G.; Dragowsky, M. R.;
   Duba, C. A.; Duncan, F. A.; Dunford, M.; Dunmore, J. A.; Earle, E. D.;
   Elliott, S. R.; Evans, H. C.; Ewan, G. T.; Farine, J.; Fergani, H.;
   Ferraris, A. P.; Fleurot, F.; Ford, R. J.; Formaggio, J. A.; Fowler,
   M. M.; Frame, K.; Frank, E. D.; Frati, W.; Gagnon, N.; Germani, J. V.;
   Gil, S.; Goldschmidt, A.; Goon, J. T. M.; Graham, K.; Grant, D. R.;
   Guillian, E.; Hahn, R. L.; Hallin, A. L.; Hallman, E. D.; Hamer,
   A. S.; Hamian, A. A.; Handler, W. B.; Haq, R. U.; Hargrove, C. K.;
   Harvey, P. J.; Hazama, R.; Heeger, K. M.; Heintzelman, W. J.; Heise,
   J.; Helmer, R. L.; Henning, R.; Hepburn, J. D.; Heron, H.; Hewett,
   J.; Hime, A.; Howard, C.; Howe, M. A.; Huang, M.; Hykaway, J. G.;
   Isaac, M. C. P.; Jagam, P.; Jamieson, B.; Jelley, N. A.; Jillings,
   C.; Jonkmans, G.; Kazkaz, K.; Keener, P. T.; Kirch, K.; Klein, J. R.;
   Knox, A. B.; Komar, R. J.; Kormos, L. L.; Kos, M.; Kouzes, R.; Krüger,
   A.; Kraus, C.; Krauss, C. B.; Kutter, T.; Kyba, C. C. M.; Labranche,
   H.; Lange, R.; Law, J.; Lawson, I. T.; Lay, M.; Lee, H. W.; Lesko,
   K. T.; Leslie, J. R.; Levine, I.; Loach, J. C.; Locke, W.; Luoma,
   S.; Lyon, J.; MacLellan, R.; Majerus, S.; Mak, H. B.; Maneira, J.;
   Marino, A. D.; Martin, R.; McCauley, N.; McDonald, A. B.; McDonald,
   D. S.; McFarlane, K.; McGee, S.; McGregor, G.; Drees, R. Meijer; Mes,
   H.; Mifflin, C.; Miknaitis, K. K. S.; Miller, M. L.; Milton, G.;
   Moffat, B. A.; Monreal, B.; Moorhead, M.; Morrissette, B.; Nally,
   C. W.; Neubauer, M. S.; Newcomer, F. M.; Ng, H. S.; Nickel, B. G.;
   Noble, A. J.; Norman, E. B.; Novikov, V. M.; Oblath, N. S.; Okada,
   C. E.; O'Keeffe, H. M.; Ollerhead, R. W.; Omori, M.; Orrell, J. L.;
   Oser, S. M.; Ott, R.; Peeters, S. J. M.; Poon, A. W. P.; Prior, G.;
   Reitzner, S. D.; Rielage, K.; Roberge, A.; Robertson, B. C.; Robertson,
   R. G. H.; Rosendahl, S. S. E.; Rowley, J. K.; Rusu, V. L.; Saettler,
   E.; Schülke, A.; Schwendener, M. H.; Secrest, J. A.; Seifert, H.;
   Shatkay, M.; Simpson, J. J.; Sims, C. J.; Sinclair, D.; Skensved,
   P.; Smith, A. R.; Smith, M. W. E.; Starinsky, N.; Steiger, T. D.;
   Stokstad, R. G.; Stonehill, L. C.; Storey, R. S.; Sur, B.; Tafirout,
   R.; Tagg, N.; Takeuchi, Y.; Tanner, N. W.; Taplin, R. K.; Thorman,
   M.; Thornewell, P. M.; Tolich, N.; Trent, P. T.; Tserkovnyak, Y. I.;
   Tsui, T.; Tunnell, C. D.; van Berg, R.; van de Water, R. G.; Virtue,
   C. J.; Walker, T. J.; Wall, B. L.; Waltham, C. E.; Tseung, H. Wan
   Chan; Wang, J. -X.; Wark, D. L.; Wendland, J.; West, N.; Wilhelmy,
   J. B.; Wilkerson, J. F.; Wilson, J. R.; Wittich, P.; Wouters, J. M.;
   Wright, A.; Yeh, M.; Zuber, K.
Bibcode: 2007PhRvC..75d5502A
Altcode: 2006nucl.ex..10020S
  This article provides the complete description of results from the
  Phase I data set of the Sudbury Neutrino Observatory (SNO). The
  Phase I data set is based on a 0.65 kiloton-year exposure of
  <SUP>2</SUP>H<SUB>2</SUB>O (in the following denoted as D<SUB>2</SUB>O)
  to the solar B8 neutrino flux. Included here are details of the SNO
  physics and detector model, evaluations of systematic uncertainties,
  and estimates of backgrounds. Also discussed are SNO's approach to
  statistical extraction of the signals from the three neutrino reactions
  (charged current, neutral current, and elastic scattering) and the
  results of a search for a day-night asymmetry in the ν<SUB>e</SUB>
  flux. Under the assumption that the B8 spectrum is undistorted,
  the measurements from this phase yield a solar ν<SUB>e</SUB> flux of
  ϕ(ν<SUB>e</SUB>)=1.76<SUB>-0.05</SUB><SUP>+0.05</SUP>(stat.)<SUB>-0.09</SUB><SUP>+0.09</SUP>(syst.)×10<SUP>6</SUP>
  cm<SUP>-2</SUP> s<SUP>-1</SUP> and a non-ν<SUB>e</SUB> component of
  ϕ(ν<SUB>μτ</SUB>)=3.41<SUB>-0.45</SUB><SUP>+0.45</SUP>(stat.)<SUB>-0.45</SUB><SUP>+0.48</SUP>(syst.)×10<SUP>6</SUP>
  cm<SUP>-2</SUP> s<SUP>-1</SUP>. The sum of these components provides a
  total flux in excellent agreement with the predictions of standard solar
  models. The day-night asymmetry in the ν<SUB>e</SUB> flux is found to
  be A<SUB>e</SUB>=7.0±4.9(stat.)<SUB>-1.2</SUB><SUP>+1.3</SUP>%(syst.),
  when the asymmetry in the total flux is constrained to be zero.

Title: Magnetic Properties of Metric Noise Storms Associated with
    Coronal Mass Ejections
Authors: Wen, Ya-Yuan; Wang, Jing-Xiu; Zhang, Yu-Zong
Bibcode: 2007ChJAA...7..265W
Altcode:
  Using Nançay Radioheliograph (NRH) imaging observations, combined
  with SOHO/Michelson Doppler Imager (MDI) magnetogram observations and
  coronal magnetic field extrapolation, we studied the magnetic nature
  of metric noise storms that are associated with coronal mass ejections
  (CMEs). Four events are selected: the events of 2000 July 14, 2001
  April 26, 2002 August 16 and 2001 March 28. The identified noise storm
  sources cover or partially cover the active regions (ARs), but the
  centers of storm sources are offset from the ARs. Using extrapolated
  magnetic field lines, we find that the noise storm sources trace the
  boundary between the open and closed field lines. We demonstrate that
  the disappearance of noise storm source is followed by the appearance of
  the burst source. The burst sources spread on the solar disk and their
  distributions correspond to the extent of the CME in LASCO C2 field of
  view. All the SOHO/Extreme Ultraviolet Imaging Telescope (EIT) dimmings
  associated with noise storm sources are located at the periphery of
  noise storms where the magnetic lines of force were previously closed
  and low-lying. When the closed field becomes partially or fully open,
  the basic configurations of noise storm sources are changed, then
  the noise storm sources are no longer observed. These observations
  provide the information that the variations of noise storms manifest
  the restructuring or reconfiguring of the coronal magnetic field.

Title: Investigating the Nuclear Obscuration in Two Types of Seyfert
    2 Galaxies
Authors: Shu, X. W.; Wang, J. X.; Jiang, P.; Fan, L. L.; Wang, T. G.
Bibcode: 2007ApJ...657..167S
Altcode: 2006astro.ph..3338S
  We build a large sample of Seyfert 2 galaxies (Sy2s) with both
  optical spectropolarimetric and X-ray data available, in which
  29 of the Sy2s have a detection of polarized broad emission
  lines (PBLs) and 25 do not. We find that for luminous Sy2s with
  L<SUB>[OIII</SUB>&gt;10<SUP>41</SUP> ergs s<SUP>-1</SUP>, sources with
  PBLs have smaller X-ray absorption column densities in comparison to
  those without PBLs (at a 92.3% confidence level): most of the Sy2s
  with N<SUB>H</SUB>&lt;10<SUP>23.8</SUP> cm<SUP>-2</SUP> show PBLs
  (86%; 12 out of 14), while the fraction is much smaller for sources
  with heavier obscuration (54%; 15 out of 28). The confidence level
  of the difference in absorption bounces up to 99.1% when using the
  thickness (``T'') ratio (F<SUB>2-10keV</SUB>/F<SUB>[OIII</SUB>) as an
  indicator. We rule out observation or selection bias as the origin for
  the difference. Our results, for the first time with high statistical
  confidence, show that, in additional to the activity of the nuclei,
  the nuclear obscuration also plays an important role in the visibility
  of PBLs in Sy2s. These results can be interpreted in the framework of
  the unified model. We can reach these results in the unified model if
  (1) the absorption column density is higher at large inclinations and
  (2) the scattering region is obscured at large inclinations.

Title: Most Hard-X-Ray-Selected Quasars in the Chandra Deep Fields
    are Obscured
Authors: Wang, J. X.; Jiang, P.; Zheng, Z. Y.; Tozzi, P.; Norman,
   C.; Giacconi, R.; Gilli, R.; Hasinger, G.; Kewley, L.; Mainieri,
   V.; Nonino, M.; Rosati, P.; Streblyanska, A.; Szokoly, G.; Zirm, A.;
   Zheng, W.
Bibcode: 2007ApJ...657...95W
Altcode: 2006astro.ph.11251W
  Measuring the population of obscured quasars is one of the key issues
  in understanding the evolution of active galactic nuclei (AGNs). With
  a redshift completeness of 99%, the X-ray sources detected in the
  Chandra Deep Field South (CDF-S) provide the best sample for this
  issue. In this paper, we study the population of obscured quasars in
  CDF-S by choosing the 4-7 keV selected sample, which is less biased
  by the intrinsic X-ray absorption. The 4-7 keV band-selected samples
  also filter out most of the X-ray-faint sources with too few counts,
  for which the measurements of N<SUB>H</SUB> and L<SUB>X</SUB> have
  very large uncertainties. Simply adopting the best-fit L<SUB>2-10
  keV</SUB> and N<SUB>H</SUB>, we find that 71%+/-19% (20 out of 28)
  of the quasars (with intrinsic L<SUB>2-10 keV</SUB>&gt;10<SUP>44</SUP>
  ergs s<SUP>-1</SUP>) are obscured with N<SUB>H</SUB>&gt;10<SUP>22</SUP>
  cm<SUP>-2</SUP>. Taking into account the uncertainties in the
  measurements of both N<SUB>H</SUB> and L<SUB>X</SUB>, conservative lower
  and upper limits for the fraction are 54% (13 out 24) and 84% (31 out
  37). In the Chandra Deep Field North, the number is 29%; however, this
  is mainly due to the redshift incompleteness. We estimate a fraction
  of ~50%-63% after correcting for the redshift incompleteness with a
  straightforward approach. Our results robustly confirm the existence
  of a large population of obscured quasars.

Title: Commission 10: Solar Activity
Authors: Melrose, Donald B.; Klimchuk, James A.; Benz, A. O.; Craig,
   I. J. D.; Gopalswamy, N.; Harrison, R. A.; Kozlovsky, B. Z.; Poletto,
   G.; Schrijver, K. J.; van Driel-Gesztelyi, L.; Wang, J. -X.
Bibcode: 2007IAUTA..26...75M
Altcode:
  Commission 10 aims at the study of various forms of solar activity,
  including networks, plages, pores, spots, fibrils, surges, jets,
  filaments/prominences, coronal loops, flares, coronal mass ejections
  (CMEs), solar cycle, microflares, nanoflares, coronal heating etc.,
  which are all manifestation of the interplay of magnetic fields and
  solar plasma. Increasingly important is the study of solar activities
  as sources of various disturbances in the interplanetary space
  and near-Earth "space weather".Over the past three years a major
  component of research on the active Sun has involved data from the
  RHESSI spacecraft. This review starts with an update on current and
  planned solar observations from spacecraft. The discussion of solar
  flares gives emphasis to new results from RHESSI, along with updates on
  other aspects of flares. Recent progress on two theoretical concepts,
  magnetic reconnection and magnetic helicity is then summarized, followed
  by discussions of coronal loops and heating, the magnetic carpet
  and filaments. The final topic discussed is coronal mass ejections
  and space weather.The discussions on each topic is relatively brief,
  and intended as an outline to put the extensive list of references
  in context.The review was prepared jointly by the members of the
  Organizing Committee, and the names of the primary contributors to
  the various sections are indicated in parentheses.

Title: Eruption of an Active-Region Filament Driven by an Emerging
    Bipole
Authors: Jiang, Yun-Chun; Shen, Yuan-Deng; Wang, Jing-Xiu
Bibcode: 2007ChJAA...7..129J
Altcode:
  A section of an S-shaped filament underwent an eruption in a
  sigmoidal active region (AR 8027) with S-shaped coronal structure,
  which was clearly driven by a bipole emerging below the NW end of
  the filament. The bipole with two separating poles showed typical
  characteristics of emerging flux region (EFR) and its axis rotated
  counterclockwise. Two cancelling magnetic features (CMFs) were formed
  between the two poles and adjacent flux with opposite polarity and
  substantial flux cancellation occurred in them. Along with the bipole
  emergence the filament was strongly disturbed. Just before the filament
  eruption, two X-ray loops overlying the filament brightened, an axial
  X-ray structure and then a cusp structure appeared. During the eruption
  first the whole filament rose and then its SE end broke away from the
  chromosphere, while its NW end remained stationary. Helical structure
  and motion were observed in the filament body and downward mass motion
  in the two ends. After the eruption, a major part of the filament
  remained and slowly returned to quiescence, and an X-ray arcade and an
  axial structure formed. These observations suggest that the eruption
  resulted from the interaction between the bipole and the overlying
  loops. We provide evidence that steady photospheric reconnection between
  their footprints took place in the two CMFs during the bipole emergence.

Title: VizieR Online Data Catalog: X-ray properties of AGN in CDFS
    (Tozzi+, 2006)
Authors: Tozzi, P.; Gilli, R.; Mainieri, V.; Norman, C.; Risaliti,
   G.; Rosati, P.; Bergeron, J.; Borgani, S.; Giacconi, R.; Hasinger,
   G.; Nonino, M.; Streblyanska, A.; Szokoly, G.; Wang, J. X.; Zheng, W.
Bibcode: 2007yCat..34510457T
Altcode:
  We present a detailed X-ray spectral analysis of the sources in the
  1Ms catalog of the Chandra Deep Field South (CDFS, J/ApJS/139/369)
  taking advantage of optical spectroscopy and photometric redshifts for
  321 extragalactic sources out of the total sample of 347 sources. As
  a default spectral model, we adopt a power law with slope Gamma with
  an intrinsic redshifted absorption N<SUB>H</SUB>, a fixed Galactic
  absorption and an unresolved Fe emission line. For 82 X-ray bright
  sources, we are able to perform the X-ray spectral analysis leaving
  both Gamma and N<SUB>H</SUB> free. <P />(1 data file).

Title: Periodicities in solar filament activity
Authors: Song, W. B.; Wang, J. X.
Bibcode: 2007AcASn..48...29S
Altcode:
  By using the Meudon filament catalogues we reconstruct a daily sequence
  of filament counts from July 1957 to December 2004 and perform a
  periodicity analysis with the methods of Scargle periodogram and Morlet
  wavelet transform. As a result, four prominent periods are found around
  1557, 1141, 795 and 367 days. We analyze their temporal variabilities
  in detail and discuss some typical ones' phases, physical implications
  and mutual relations briefly.

Title: Two Successive Coronal Mass Ejections Driven by the Kink and
    Drainage Instabilities of an Eruptive Prominence
Authors: Zhou, G. P.; Wang, J. X.; Zhang, J.; Chen, P. F.; Ji, H. S.;
   Dere, K.
Bibcode: 2006ApJ...651.1238Z
Altcode:
  We describe a clear case of the initiation of a propagating bright arc
  and a CME on 2002 December 28, which were associated with an eruptive
  prominence. In EIT 304 and 195 Å images, a very long filament showed
  evidence of severe twisting in one of its fragments, which appeared as a
  prominence on December 26; then, the prominence showed the conversion of
  its twist into writhe. Two days later, the prominence displayed a slow
  rising motion for hours. Internal twisting and mass motion took place
  before the rapid acceleration and final eruption. The propagating bright
  arc and the following CME corresponded to the early rising and the
  subsequently eruptive phases of the prominence, respectively. Signatures
  of magnetic reconnection, i.e., a cusp structure and postflare loops
  in EUV wave bands and hard X-ray sources in the corona, were observed
  after the prominence eruption. It appears that the kink instability
  and the mass drainage in the prominence played key roles in triggering
  the initiation of the CME. However, the rather impulsive acceleration
  of the CME resulted from magnetic reconnection beneath the filament.

Title: 3D Topology Structure of Coronal Magnetic Field
Authors: Zhao, H.; Wang, J. X.; Zhang, J.; Xiao, C. J.
Bibcode: 2006IAUJD...3E..40Z
Altcode:
  We use the Poincaré index of isolated null-points in vector field
  to strictly identify 3D null-points in coronal magnetic fields
  reconstructed from the observed vector magnetogram of several important
  active regions. Base on the null-points we identified, we reveal the
  essential topology skeletons of 3D coronal magnetic fields. Comparing
  these topology skeletons with images of H-alpha, EIT, TRACE and X-ray,
  we find 3D topology structures of coronal magnetic fields are closely
  associated with solar flares and CMEs. We also find indication of
  3D magnetic reconnection by studying temporal series of 3D topology
  structures of solar magnetic fields. To thoroughly investigate 3D
  topology structures of coronal magnetic fields is a key to understand
  the physical mechanism of solar activity.

Title: On the Fraction of X-Ray-obscured Quasars in the Local Universe
Authors: Wang, J. X.; Jiang, P.
Bibcode: 2006ApJ...646L.103W
Altcode: 2006astro.ph..6333W
  Recent wide-area hard X-ray and soft gamma-ray surveys have shown that
  the fraction of X-ray-obscured active galactic nuclei (AGNs) in the
  local universe significantly decreases with intrinsic luminosity. In
  this Letter we point out that two corrections have to be made to
  the samples: (1) radio-loud AGNs have to be excluded, since their
  X-ray emission might be dominated by the jet component, and (2)
  Compton-thick sources have to be excluded too, since their hard X-ray
  and soft gamma-ray emission are also strongly attenuated by Compton
  scattering. The soft gamma-ray-selected AGN samples obtained by Swift
  and INTEGRAL provide the best opportunity to study the fraction of
  obscured AGNs in the local universe in the least biased way. We choose
  these samples to check if the corrections could alter the above result
  on the fraction of obscured AGNs. We find that before the corrections
  both samples show significant anticorrelation between L<SUB>X</SUB>
  and N<SUB>H</SUB>, indicating an obvious decrease in the fraction of
  obscured AGNs with luminosity. However, after the corrections, we find
  only marginal evidence of anticorrelation (at the 98% confidence level)
  in the Swift sample and no evidence at all in the INTEGRAL sample,
  which consists of a comparable number of objects. We conclude that
  current samples only show a marginal decrease in the fraction of
  obscured AGNs in the local universe and that much larger samples are
  required in order to reach a more robust conclusion.

Title: Solar radiation pressure models for the GPS satellites
Authors: Chen, J. P.; Wang, J. X.
Bibcode: 2006AcASn..47..310C
Altcode:
  The largest error in currently used for GPS orbit models is due to the
  effect of solar radiation pressure (SRP). Over the last a few years
  many improvement were made in modeling the orbits of GPS satellites
  within the IGS. One of the most important factors for the improvement
  is the perfect of SRP models. The main SRP models currently used for
  GPS satellites is presented. Using different models, it can get the
  performance of the models in satellite orbit determining. The results
  show that new models developed by Bern University gain almost an order
  of magnitude better than that of the other traditional models.

Title: In situ evidence for the structure of the magnetic null in
    a 3D reconnection event in the Earth's magnetotail
Authors: Xiao, C. J.; Wang, X. G.; Pu, Z. Y.; Zhao, H.; Wang, J. X.;
   Ma, Z. W.; Fu, S. Y.; Kivelson, M. G.; Liu, Z. X.; Zong, Q. G.;
   Glassmeier, K. H.; Balogh, A.; Korth, A.; Reme, H.; Escoubet, C. P.
Bibcode: 2006NatPh...2..478X
Altcode: 2006physics...6014X
  Magnetic reconnection is one of the most important processes
  in astrophysical, space and laboratory plasmas. Identifying the
  structure around the point at which the magnetic field lines break and
  subsequently reform, known as the magnetic null point, is crucial to
  improving our understanding of reconnection. But owing to the inherently
  three-dimensional nature of this process, magnetic nulls are only
  detectable through measurements obtained simultaneously from at least
  four points in space. Using data collected by the four spacecraft of
  the Cluster constellation as they traversed a diffusion region in the
  Earth's magnetotail on 15 September 2001, we report here the first
  in situ evidence for the structure of an isolated magnetic null. The
  results indicate that it has a positive-spiral structure whose spatial
  extent is of the same order as the local ion inertial length scale,
  suggesting that the Hall effect could play an important role in 3D
  reconnection dynamics.

Title: On the X-Ray Baldwin Effect for Narrow Fe Kα Emission Lines
Authors: Jiang, P.; Wang, J. X.; Wang, T. G.
Bibcode: 2006ApJ...644..725J
Altcode: 2006astro.ph..3339J
  Most active galactic nuclei (AGNs) exhibit a narrow Fe Kα line at
  ~6.4 keV in the X-ray spectra, due to the fluorescent emission from
  cold material far from the inner accretion disk. Using XMM-Newton
  observations, Page et al. found that the equivalent width (EW)
  of the narrow Fe Kα line decreases with increasing luminosity
  (EW~L<SUP>-0.17+/-0.08</SUP>), suggesting a decrease in the
  covering factor of the material emitting the line (presumably the
  torus). By combining the archival Chandra HETG observations of 34
  type 1 AGNs with XMM observations in the literature, we build a
  much larger sample with 101 AGNs. We find a similar X-ray Baldwin
  effect in the sample (EW~L<SUP>-0.2015+/-0.0426</SUP>) however,
  we note that the anticorrelation is dominated by the radio-loud
  AGNs in the sample, whose X-ray spectra might be contaminated by
  the relativistic jet. Excluding the radio-loud AGNs, we find a much
  weaker anticorrelation (EW~L<SUP>-0.1019+/-0.0524</SUP>). We present
  Monte Carlo simulations showing that such a weak anticorrelation can
  be attributed to the relative short timescale variations of the X-ray
  continuum.

Title: Catastrophic Behavior of Multiple Coronal Flux Rope System
Authors: Ding, J. Y.; Hu, Y. Q.; Wang, J. X.
Bibcode: 2006SoPh..235..223D
Altcode:
  A major solar active event called Bastille Day Event occurred in AR
  9077 on July 14, 2000. Simultaneous occurrence of a filament eruption,
  a flare and a coronal mass ejection was observed in this event. Previous
  analyses of this event show that before the event, there existed an
  activation and eruption of a huge trans-equatorial filament, which
  might play a crucial role in triggering the Bastille Day event. This
  implies that independent flux systems are closely related to and affect
  each other, which has encouraged us to investigate the catastrophic
  behavior of a multiple coronal flux rope system with the use of a
  2.5-D time-dependent MHD model. A force-free field that contains three
  separate coronal flux ropes is taken to be the initial state. Starting
  from this state, we increase either the annular or the axial flux of a
  certain flux rope to examine the catastrophic behavior of the system in
  two regimes, the ideal MHD regime and the resistive MHD regime. It is
  found that a catastrophe occurs if the flux exceeds a certain critical
  value, or the magnetic energy of the system exceeds a certain threshold:
  the rope of interest breaks away from the base and escapes to infinity,
  leaving a current sheet below. Moreover, the destiny of the remainder
  flux ropes relies on whether reconnection takes place across the current
  sheet. In the ideal MHD regime, i.e., in the absence of reconnection,
  these ropes remain to be attached to the base in equilibrium, whereas in
  the resistive MHD regime they abruptly erupt upward during reconnection
  and escape to infinity. Reconnection causes the field lines to close
  back to the base and thus changes the background field outside the
  attached flux ropes in such a way that the constraint on these ropes
  is substantially relaxed and the corresponding catastrophic energy
  threshold is reduced accordingly, leading to a catastrophic eruption
  of these ropes. Since magnetic reconnection is generally inevitable
  when a current sheet forms and develops through an eruption of one
  flux rope, the eruption of this flux rope must lead to an eruption of
  the others. This provides an example to demonstrate the interaction
  between several independent magnetic flux systems in different regions,
  as implied by the Bastille Day event, and may serve as a possible
  mechanism for sympathetic events occurring on the Sun.

Title: X-ray spectral properties of active galactic nuclei in the
    Chandra Deep Field South
Authors: Tozzi, P.; Gilli, R.; Mainieri, V.; Norman, C.; Risaliti,
   G.; Rosati, P.; Bergeron, J.; Borgani, S.; Giacconi, R.; Hasinger,
   G.; Nonino, M.; Streblyanska, A.; Szokoly, G.; Wang, J. X.; Zheng, W.
Bibcode: 2006A&A...451..457T
Altcode: 2006astro.ph..2127T
  We present a detailed X-ray spectral analysis of the sources in the
  1Ms catalog of the Chandra Deep Field South (CDFS) taking advantage of
  optical spectroscopy and photometric redshifts for 321 extragalactic
  sources out of the total sample of 347 sources. As a default spectral
  model, we adopt a power law with slope Γ with an intrinsic redshifted
  absorption N_H, a fixed Galactic absorption and an unresolved Fe
  emission line. For 82 X-ray bright sources, we are able to perform the
  X-ray spectral analysis leaving both Γ and N<SUB>H</SUB> free. The
  weighted mean value for the slope of the power law is &lt; Γ &gt;
  ≃ 1.75 ± 0.02, and the distribution of best fit values shows an
  intrinsic dispersion of σ_int ≃ 0.30. We do not find hints of a
  correlation between the spectral index Γ and the intrinsic absorption
  column density N_H. We then investigate the absorption distribution for
  the whole sample, deriving the N<SUB>H</SUB> values in faint sources by
  fixing Γ = 1.8. We also allow for the presence of a scattered component
  at soft energies with the same slope of the main power law, and for a
  pure reflection spectrum typical of Compton-thick AGN. We detect the
  presence of a scattered soft component in 8 sources; we also identify
  14 sources showing a reflection-dominated spectrum. The latter are
  referred to as Compton-thick AGN candidates. By correcting for both
  incompleteness and sampling-volume effects, we recover the intrinsic
  N<SUB>H</SUB> distribution representative of the whole AGN population,
  f(N_H) dN_H, from the observed one. f(N_H) shows a lognormal shape,
  peaking around log(N_H)≃ 23.1 and with σ ≃ 1.1. Interestingly, such
  a distribution shows continuity between the population of Compton-thin
  and that of Compton-thick AGN. We find that the fraction of absorbed
  sources (with N_H&gt;10<SUP>22</SUP> cm<SUP>-2</SUP>) in the sample
  is constant (at the level of about 75%) or moderately increasing with
  redshift. Finally, we compare the optical classification to the X-ray
  spectral properties, confirming that the correspondence of unabsorbed
  (absorbed) X-ray sources to optical type I (type II) AGN is accurate
  for at least 80% of the sources with spectral identification (1/3 of
  the total X-ray sample).

Title: A Non-axisymmetric Spherical α<SUP>2</SUP>-Dynamo
Authors: Jiang, Jie; Wang, Jing-Xiu
Bibcode: 2006ChJAA...6..227J
Altcode:
  Using the Chebyshev-tau method, the generation of oscillatory
  non-axisymmetric stellar magnetic fields by the α<SUP>2</SUP>-dynamo
  is studied in spherical geometry. Following the boundary conditions
  given by Schubert &amp; Zhang, the spherical α<SUP>2</SUP>-dynamo
  consists of a fully convective spherical shell with inner radius
  r<SUB>i</SUB> and outer radius r<SUB>o</SUB>. A comparison of the
  critical dynamo numbers of axisymmetric and phi-dependent modes for
  different thicknesses of the convective shell and different α-profiles
  leads to the following qualitative results: (i) when the angular factor
  of α-profile is sin<SUP>n</SUP>θ cos θ (n = 1,2,4) the solutions of
  the α<SUP>2</SUP>-dynamo are oscillatory and non-axisymmetric, (ii) the
  thinner the convective shell, the more easily is the non-axisymmetric
  mode excited and the higher is the latitudinal wave number, (iii)
  the thickness of the outer convective shell has an effect on the
  symmetries of the magnetic fields.

Title: Two-Current-Sheet Reconnection Model of Interdependent Flare
    and Coronal Mass Ejection
Authors: Zhang, Y. Z.; Wang, J. X.; Hu, Y. Q.
Bibcode: 2006ApJ...641..572Z
Altcode: 2006astro.ph..1231Z
  Time-dependent resistive magnetohydrodynamic simulations are carried
  out to study a flux rope eruption caused by magnetic reconnection
  with implication in coexistent flare-CME (coronal mass ejection)
  events. An early result obtained in a recent analysis of double
  catastrophe of a flux rope system is used as the initial condition,
  in which an isolated flux rope coexists with two current sheets:
  a vertical one below and a transverse one above the flux rope. The
  flux rope erupts when reconnection takes place in the current sheets,
  and the flux rope dynamics depends on the reconnection sequence in the
  two current sheets. Three cases are discussed: reconnection occurs (1)
  simultaneously in the two current sheets, (2) first in the transverse
  one and then in the vertical one, and (3) in an order opposite that of
  case 2. Such a two-current-sheet reconnection exhibits characteristics
  of both magnetic breakout for CME initiation and the standard flare
  model. We argue that both breakout-like and tether-cutting reconnections
  could be important for CME eruptions and associated surface activities.

Title: Transequatorial Filament Eruption and Its Link to a Coronal
    Mass Ejection
Authors: Wang, Jing-Xiu; Zhou, Gui-Ping; Wen, Ya-Yuan; Zhang, Yu-Zong;
   Wang, Hua-Ning; Deng, Yuan-Yong; Zhang, Jun; Harra, Louise K.
Bibcode: 2006ChJAA...6..247W
Altcode:
  We revisit the Bastille Day flare/CME Event of 2000 July 14, and
  demonstrate that this flare/CME event is not related to only one single
  active region (AR). Activation and eruption of a huge transequatorial
  filament are seen to precede the simultaneous filament eruption and
  flare in the source active region, NOAA AR 9077, and the full halo-CME
  in the high corona. Evidence of reconfiguration of large-scale magnetic
  structures related to the event is illustrated by SOHO EIT and Yohkoh
  SXT observations, as well as, the reconstructed 3D magnetic lines
  of force based on the force-free assumption. We suggest that the AR
  filament in AR 9077 was connected to the transequatorial filament. The
  large-scale magnetic composition related to the transequatorial filament
  and its sheared magnetic arcade appears to be an essential part of the
  CME parent magnetic structure. Estimations show that the filament-arcade
  system has enough magnetic helicity to account for the helicity carried
  by the related CMEs. In addition, rather global magnetic connectivity,
  covering almost all the visible range in longitude and a huge span in
  latitude on the Sun, is implied by the Nançay Radioheliograph (NRH)
  observations. The analysis of the Bastille Day event suggests that
  although the triggering of a global CME might take place in an AR,
  a much larger scale magnetic composition seems to be the source of
  the ejected magnetic flux, helicity and plasma. The Bastille Day
  event is the first described example in the literature, in which a
  transequatorial filament activity appears to play a key role in a
  global CME. Many tens of halo-CME are found to be associated with
  transequatorial filaments and their magnetic environment.

Title: Large-scale source regions of earth-directed coronal mass
    ejections
Authors: Zhou, G. P.; Wang, J. X.; Zhang, J.
Bibcode: 2006A&A...445.1133Z
Altcode:
  Based on SOHO/MDI, EIT, Yohkoh/SXT, Hα, and other relevant
  observations, we analyzed all the earth-directed halo coronal mass
  ejections (CMEs) in the interval from Mar. 1997 to Dec. 2003. A
  total of 288 earth-directed CMEs were studied and their associated
  surface activity events identified. Unlike the previous studies that
  often attributed a surface activity event or a given active region
  to a CME source region, this statistical analysis puts emphasis
  on the large-scale magnetic structures of CMEs, in which the
  CME-associated surface activity takes place. All the CMEs are found
  to be associated with large-scale source structures. The identified
  large-scale structures can be grouped into four different categories:
  extended bipolar regions (EBRs), transequatorial magnetic loops,
  transequatorial filaments and their associated magnetic structures, and
  long filaments along the boundaries of EBRs. The relative percentages
  of their associated CMEs are 36%, 40%, 13%, and 11%, respectively. The
  analysis indicates that CMEs are intrinsically associated with source
  magnetic structures on a large spatial scale.

Title: Interaction Between CME and Magnetosphere Observed by Cluster
on Nov. 6, 2001: (1) Waves Excitation
Authors: Xiao, C. J.; Song, L. T.; Pu, Z. Y.; Wang, J. X.; Liu, Z. X.;
   Glassmeier, K. -H.; Balogh, A.; Reme, H.
Bibcode: 2006IAUS..233..373X
Altcode:
  Very few in situ measurements so far show the details of the
  interactions between CME and magnetosphere. Here we report a fortuitous
  observation that the Cluster spacecraft were located at the dusk-side
  magnetopause, meandering back and forth four times between the ICME
  and the magnetosphere, and observed part process of the interaction
  between the CME and the magnetosphere. The primarily analysis showed
  that: (1) a fast ion beam other than the ambient plasma was observed
  almost perpendicular to the magnetic field; (2) The left-hand-polarized
  kinetic Alfvén waves excitation by the ion beam; and (3) the resonances
  between the kinetic Alfvén waves and part of the beam particles lead
  to the pitch angle diffusion of resonant particles and formating of
  a monospheric distribution with nearly constant kinetic energy. The
  wave-particle resonance may pay an important role in the energy transfer
  and particle exchange across the magnetopause between the magnetosheath
  and magnetosphere during the CME impulsion.

Title: A Non-axisymmetric Solar Dynamo Model
Authors: Jiang, J.; Wang, J. X.
Bibcode: 2006cosp...36..814J
Altcode: 2006cosp.meet..814J
  Increasing observations are becoming available about a weak but
  persistent non-axisymmetric magnetic field co-exist with the dominant
  axisymmetric field on the Sun It indicates non-axisymmetric magnetic
  fields play an important role in the origin of solar activities A
  nonlinear non-axisymmetric dynamo model is applied to try to give
  an explanation of this phenomenon The model is characterized by a
  solar-like internal differential rotation profile distribution of
  turbulent diffusivity and the nonlinear alpha-quench in spherical
  coordinate r theta phi Only the modes m 0 and 1 are considered and
  numerically solved as an eigenvalue problem The stable solutions can
  be found The distributions of the non-axisymmetric part of the surface
  fields and the magnetic energies as a function of time for the two
  modes are given too

Title: CMEs driven by an eruptive prominence
Authors: Zhou, G. P.; Wang, J. X.; Zhang, J.; Chen, P. F.; Ji, H. S.;
   Dere, K.
Bibcode: 2006IAUS..233..405Z
Altcode:
  A clear case on Dec. 28 2002 is presented. It is about the initiation of
  two successive CMEs, which were related to an eruptive prominence. In
  EIT 304 Å and 195 Å observations, we found a long filament severely
  twisting in a piece of its fragments, which appeared as a prominence on
  Dec. 26. Then, the prominence converted its twist into writhe. Two days
  later, the prominence displayed a slow rising motion for hours. There
  happened internal twisting and mass motion before the prominence rapid
  acceleration and final eruption. Two successive CMEs recorded by LASCO
  C2 coronagraph corresponded to the early rising and the subsequently
  eruptive phases of the prominence, respectively. Evidence of magnetic
  reconnection, i.e., a cusp structure and post-flare loops in EUV
  wavebands, and hard X-ray sources in the corona, were observed after
  the prominence disruption. It appears that the kink instability and the
  mass drainage in the prominence played important roles in triggering two
  CMEs' initiation. We suspected that the rather impulsive acceleration
  of the second CME resulted from magnetic reconnection beneath the
  prominence.

Title: The acceleration error estimates in LASCO CME measures
Authors: Wen, Y. Y.; Wang, J. X.; Maia, D.; Zhao, H.
Bibcode: 2006cosp...36.1147W
Altcode: 2006cosp.meet.1147W
  Based on the paper that the error estimates for the height measures
  grows rather fast in the first few solar radii and becomes reasonably
  flat above 5 solar radii We show here how to obtain reliable
  acceleration error estimates for the measures given in the catalog We
  show that for the fast CMEs the uncertainties in the accelerations
  are quite large when compared with the average variation within a
  particular velocity subgroup of CMEs and as such only events with very
  high acceleration can reliably be considered as accelerated For most
  events one can not decide if a particular event has positive or negative
  acceleration As a consequence and classification that separates CMEs
  according to acceleration criteria will find similar distributions for
  accelerated and decelerated CMEs but that only reflects the fact that
  the error in determining the acceleration is quit high On average we
  find that slower CMEs tend to have a positive acceleration about 1
  m s 2 at heights above 5 solar radii while the 5 faster CMEs show an
  average negative acceleration about -2 5 m s 2 as they propagate from
  5 to 30 solar radii

Title: MHD Numerical Simulation of Interdependent Flares and CMEs
Authors: Zhang, Y. Z.; Wang, J. X.; Hu, Y. Q.
Bibcode: 2006IAUS..233..130Z
Altcode:
  Using time-dependent resistive magnetohydrodynamic simulations, we study
  a flux rope eruption caused by magnetic reconnection with implication
  in coexistent flare-CME events. Without the resistance the flux rope
  system presents a double catastrophe. We use the first catastrophic
  state as the initial condition, in which an isolated flux rope coexists
  with two current sheets: a vertical one below and a transverse one
  above the flux rope. The flux rope erupts when reconnection starts
  in the current sheets, and the flux rope dynamics depends on the
  reconnection sequence in the two current sheets. We obtain three cases:
  reconnection occurs (1) simultaneously in the two current sheets,
  (2) first in the transverse one and then in the vertical, and (3)
  in an order opposite to case 2. Such a model exhibits characteristics
  of both magnetic breakout model for CME initiation and standard flare
  model. We argue that both breakout-like and tether-cutting reconnections
  may be important for CME eruptions.

Title: High-precision polarimetry design for Space Solar Telescope
Authors: Zhang, Z. Y.; Deng, Y. Y.; Hu, K. L.; Wang, D. G.; Lin,
   J. B.; Sun, Y. Z.; Wang, J. X.
Bibcode: 2006cosp...36.2864Z
Altcode: 2006cosp.meet.2864Z
  High polarization accuracy and high spatial resolution measurement
  of solar magnetic field is the most important mission of Space Solar
  Telescope Although there is no seeing induced error in the outer
  space the mass flow and evolution in the solar atmosphere may become
  the main source of false polarization signals To reduce this source
  of polarization errors a high-speed polarimetry is required In this
  paper we present our newly designed polarimeter based on high-speed
  electro-optical modulation We employ Mueller Matrix to analyses
  the polarization characteristics of optical elements and evaluate
  the polarization errors By these discussions we also determine the
  requirements to the imaging process system of SST

Title: Solar proton spectrum and acceleration during the 20 January
    2005 flare
Authors: Wang, R. G.; Wang, J. X.
Bibcode: 2006cosp...36.1856W
Altcode: 2006cosp.meet.1856W
  A extreme solar cosmic ray event was broken out on 20 January 2005
  It was not only the most intense solar energetic particle SEP event
  measured by GOES satellites since 1976 but also the largest ground level
  enhancement GLE recorded in neutron monitors since 1956 We present the
  solar proton energy spectra of this event data from GOES measurements in
  multi-channels of energy These spectra are well fit by a double power
  law form It was shown that the January 20 event had the hardest energy
  spectrum during solar cycle 23 and the highest fluxes for above 30 MeV
  protons in past 30 years We examine variations of the spectral index
  from -1 4 to -0 8 within the rise phase of proton intensity Combing
  X-ray radio emission and CME observation as well as available neutron
  monitor data relativistic proton acceleration and travel is discussed
  It seems to imply that the first arrival relativistic protons are
  released in low corona and accelerated up to GeV within minutes This
  impulsive high energy process more likely associated with solar flare
  instead of CME

Title: Large geomagnetic storms of extreme solar event periods in
    solar cycle 23
Authors: Wang, R. G.; Wang, J. X.
Bibcode: 2006cosp...36.1855W
Altcode: 2006cosp.meet.1855W
  At the duration of extreme solar events solar eruption associated
  with big flares or and energetic coronal mass ejections CMEs can not
  only make high energy particles acceleration but also give rise to
  large geomagnetic storms which have significant effects on the Earth
  s environment and human life Around 14 solar cosmic ray ground level
  enhancement GLE events in solar cycle 23 we examine the cosmic ray
  variations solar wind speeds ion densities interplanetary magnetic
  fields and geomagnetic disturbance storm time indices Dst We find that
  all but one of GLEs are always followed by a geomagnetic storm with Dst
  leq -50 nT within 1-5 days later Most 10 14 geomagnetic storms have Dst
  index leq -100 nT suggesting that GLE event prediction of geomagnetic
  storms is 93 for moderate storms and 71 for large storms More than
  half 57 Dst depressions are simultaneously accompanied by cosmic ray
  decreases and other Dst variabilities are without clear cosmic ray
  deceases We also investigated the interplanetary plasma features during
  GLE events Most geomagnetic storm correspond significant periods of
  southward B z and in close to 80 of the cases that the B z was first
  northward then turning southward after storm sudden commencement
  SSC Plasma flow speed ion number density and interplanetary plasma
  temperature near 1 AU also have a peak at interplanetary shock arrival
  Solar cause and energetic particle signatures of large geomagnetic
  storms are discussed

Title: Homologous emerging flux and associated solar activity
Authors: Zhou, G. P.; Wang, J. X.
Bibcode: 2006cosp...36.2906Z
Altcode: 2006cosp.meet.2906Z
  There are 69 GOES X-ray flares produced in the active regions ARs
  10486 and 10488 during the famous Oct -Nov 2003 solar event Among them
  the X28 flare in AR10488 on Nov 04 2003 may have been the largest
  X-ray event since observations began in 1976 Part of the associated
  large flare CMEs form magnetic clouds in the interplanetary space By
  investigating the photosphere magnetograms we find that the emerging
  flux in AR10486 10488 10489 10491 and 10492 appear homologous The
  homologous behaviors are further confirmed by the evidence from the
  sub-photospheric flow maps vertical velocity and meridional vorticity
  as well as these ARs evolutions in MDI synoptic charts We also find that
  there is large-scale magnetic connectivity among these ARs whether from
  EIT images or from the global magnetic force lines reconstructed by
  the potential extrapolation which indicate these referred ARs are not
  isolated each other The ARs are probably involved in a same topological
  magnetic system since we find a predominant negative helicity sign in
  these ARs and their associated magnetic clouds With more analysis on
  the other observations in TRACE RHESSI GOES and so on it is speculated
  that the associated flares CMEs initiate during the evolutions of this
  topological isolated magnetic system especially when it interacted
  with the other environmental flux

Title: The detection of "magnetic element"---why we need an one-meter
    Space Solar Telescope
Authors: Deng, Y. Y.; Wang, J. X.; Ai, G. X.
Bibcode: 2006cosp...36..942D
Altcode: 2006cosp.meet..942D
  The nature of magnetic element the elemental structure of solar
  magnetic field is one of the most important mysteries in solar physics
  The intrinsic properties of magnetic element such as field strength
  filling factor spatial scale are unknown yet though the history of
  solar magnetic measurement can go back to one hundred years ago With
  the development of technology solar physicists have made a lots of
  attempts to resolve the magnetic element directly For example with
  the help of a set of techniques adaptive optics correlation tracker
  image reconstruction etc the one-meter Swedish Solar Telescope in the
  Canary Islands has nearly reached its diffraction-limit resolution
  sim 0 18 630 25nm which roughly match the spatial-scale requirement
  of magnetic element detection However none current-used telescope can
  resolve magnetic element at this moment yet as spatial resolution is
  just one of the requirements of magnetic element detection In this
  paper the requirements of magnetic element detection will be discussed
  By these discussions we know that the spatial resolution temporal
  resolution and magnetic sensitivity are all important The proposed
  Space Solar Telescope an one-meter Chinese space telescope can match
  these requirements

Title: Solar <SUP>3</SUP>He-rich events and abnormal enhancements
    of heavy-ion isotopes accelerated in two stages
Authors: Zhang, T. X.; Wang, J. X.; Tan, A.
Bibcode: 2005JGRA..11012111Z
Altcode:
  Heating and acceleration of neon (<SUP>20</SUP>Ne), magnesium
  (<SUP>24</SUP>Mg), and their rare isotopes (<SUP>22</SUP>Ne and
  <SUP>26</SUP>Mg) in solar <SUP>3</SUP>He-rich events are investigated
  according to the two-stage acceleration mechanism. It is shown
  that <SUP>20</SUP>Ne<SUP>+8</SUP>, <SUP>22</SUP>Ne<SUP>+9</SUP>,
  <SUP>24</SUP>Mg<SUP>+10</SUP>, and <SUP>26</SUP>Mg<SUP>+11</SUP>
  can be preferentially heated by H-cyclotron waves with a frequency
  close to twice the <SUP>3</SUP>He-cyclotron frequency that
  also heat <SUP>3</SUP>He, through the third harmonic cyclotron
  resonance. If the initial electron temperature is in the range of
  ∼2-10 MK, the abundance ratios <SUP>22</SUP>Ne/<SUP>20</SUP>Ne and
  <SUP>26</SUP>Mg/<SUP>24</SUP>Mg in high-energy particles due to the
  second-stage acceleration can be enhanced by a factor of ∼2-6 relative
  to the solar corona, which are consistent with the measurements of the
  University of Maryland particle instrument on the Solar Anomalous and
  Magnetospheric Particle Explorer and the Ultra Lower Energy Isotope
  Spectrometer particle instrument on the Advanced Composition Explorer.

Title: A New Method of Identifying 3D Null Points in Solar Vector
    Magnetic Fields
Authors: Zhao, Hui; Wang, Jing-Xiu; Zhang, Jun; Xiao, Chi-Jie
Bibcode: 2005ChJAA...5..443Z
Altcode:
  Employing the Poincaré index of isolated null-points in a vector field,
  we worked out a mathematical method of searching for 3D null-points in
  coronal magnetic fields. After introducing the relevant differential
  topology, we test the method by using the analytical model of Brown
  &amp; Priest. The location of null-point identified by our method
  coincides precisely with the analytical solution. Finally we apply
  the method to the 3D coronal magnetic fields reconstructed from an
  observed MDI magnetogram of a super-active region (NOAA 10488). We
  find that the 3D null-point seems to be a key element in the magnetic
  topology associated with flare occurrence.

Title: Relativistic Outflow in CXOCDFS J033260.0-274748
Authors: Wang, J. X.; Wang, T. G.; Tozzi, P.; Giacconi, R.; Hasinger,
   G.; Kewley, L.; Mainieri, V.; Nonino, M.; Norman, C.; Streblyanska,
   A.; Szokoly, G.; Yaqoob, T.; Zirm, A.
Bibcode: 2005ApJ...631L..33W
Altcode: 2005astro.ph..8225W
  In this Letter we report the detection of a strong and extremely
  blueshifted X-ray absorption feature in the 1 Ms Chandra
  spectrum of CXOCDFS J033260.0-274748, a quasar at z=2.579 with
  L<SUB>2-10keV</SUB>~4×10<SUP>44</SUP> ergs s<SUP>-1</SUP>. The broad
  absorption feature at ~6.3 keV in the observed frame can be fitted
  either as an absorption edge at 20.9 keV or as a broad absorption line
  at 22.2 keV rest frame. The absorber has to be extremely ionized with
  an ionization parameter ξ~10<SUP>4</SUP>, and a high column density,
  N<SUB>H</SUB>&gt;5×10<SUP>23</SUP> cm<SUP>-2</SUP>. We reject the
  possibility of a statistical or instrumental artifact. The most likely
  interpretation is an extremely blueshifted broad absorption line or
  absorption edge, due to H or He-like iron in a relativistic jetlike
  outflow with bulk velocity of ~0.7c-0.8c. Similar relativistic outflows
  have been reported in the X-ray spectra of several other AGNs in the
  past few years.

Title: Progress in the studies on a relic solar magnetic field
Authors: Song, Wen-Bin; Wang, Jing-Xiu
Bibcode: 2005PABei..23..205S
Altcode:
  It is really possible that the Sun possesses a relic magnetic field
  of the pre-main sequence epoch in its radiative core. Due to a stably
  stratified fluid and an extremely high electrical conductivity in the
  solar interior, a relic solar magnetic field can survive for a very
  long time. A relic field can help us to explain many asymmetries in
  solar activities, such as the north-south asymmetries of solar magnetic
  activities, active longitudes and holes, low-latitude coronal holes,
  Maunder minimum, etc. In addition it can affect the distribution and
  evolution of solar surface magnetic field by changing the boundary
  conditions of solar dynamo. This paper focuses on the introduction
  of recent progress and issues in observations and theories of relic
  solar magnetic field. Some unresolved problems and highlights are
  also discussed.

Title: A study of the north-south asymmetry of solar photospheric
    magnetic flux
Authors: Song, Wen-bin; Wang, Jing-xiu; Ma, Xia
Bibcode: 2005ChA&A..29..274S
Altcode: 2005ChA&A..29..274W
  Statistical characteristics of the variation of the North-South
  asymmetry of solar photospheric magnetic flux in 1978-2002 are
  systematically studied, and they are found to be related to the
  cycle of solar activity. The degree of the asymmetry during the
  minimum of solar activity is obviously higher than that during the
  maximum of solar activity. Moreover, the change of magnetic flux is
  always accompanied by a gradual shift of dominance from the northern
  hemisphere in the ascending phase to the southern hemisphere in the
  descending phase. A wavelet transform is used to make a detailed probe
  of possible periodicities in the variation of the North-South asymmetry.

Title: Resonant Heating of Ions by Parallel Propagating Alfvén
    Waves in Solar Coronal Holes
Authors: Zhang, Tian-Xi; Wang, Jing-Xiu; Xiao, Chi-Jie
Bibcode: 2005ChJAA...5..285Z
Altcode:
  Resonant heating of H, O<SUP>+5</SUP>, and Mg<SUP>+9</SUP> by parallel
  propagating ion-cyclotron Alfvén waves in solar coronal holes at a
  heliocentric distance is studied using the heating rate derived from
  the quasilinear theory. It is shown that the particle-Alfvén-wave
  interaction is a significant microscopic process. The temperatures
  of the ions are rapidly increased up to the observed order in only
  microseconds, which implies that simply inserting the quasilinear
  heating rate into the fluid/MHD energy equation to calculate the
  radial dependence of ion temperatures may cause errors as the time
  scales do not match. Different species ions are heated by Alfvén
  waves with a power law spectrum in approximately a mass order. To heat
  O<SUP>+5</SUP> over Mg<SUP>+9</SUP> as measured by the Ultraviolet
  Coronagraph Spectrometer (UVCS) in the solar coronal hole at a region
  gtrsim1.9R<SUB>odot</SUB>, the energy density of Alfvén waves with a
  frequency close to the O<SUP>+5</SUP>-cyclotron frequency must be at
  least double of that at the Mg<SUP>+9</SUP>-cyclotron frequency. With
  an appropriate wave-energy spectrum, the heating of H, O<SUP>+5</SUP>
  and Mg<SUP>+9</SUP> can be consistent with the UVCS measurements in
  solar coronal holes at a heliocentric distance.

Title: VizieR Online Data Catalog: Chandra Deep Field-South: Optical
    spectroscopy (Szokoly+, 2004)
Authors: Szokoly, G. P.; Bergeron, J.; Hasinger, G.; Lehmann, I.;
   Kewley, L.; Mainieri, V.; Nonino, M.; Rosati, P.; Giacconi, R.; Gilli,
   R.; Gilmozzi, R.; Norman, C.; Romaniello, M.; Schreier, E.; Tozzi,
   P.; Wang, J. X.; Zheng, W.; Zirm, A.
Bibcode: 2005yCat..21550271S
Altcode:
  We present the results of our spectroscopic follow-up program of
  the X-ray sources detected in the 942ks exposure of the Chandra Deep
  Field-South (CDFS). A total of 288 possible counterparts were observed
  at the VLT with the FORS1/FORS2 spectrographs for 251 of the 349 Chandra
  sources (including three additional faint X-ray sources). Spectra and
  R-band images are shown for all the observed sources and R-K colors are
  given for most of them. Spectroscopic redshifts were obtained for 168
  X-ray sources, of which 137 have both reliable optical identification
  and redshift estimate (including 16 external identifications). The
  R&lt;24 observed sample comprises 161 X-ray objects (181 optical
  counterparts), and 126 of them have unambiguous spectroscopic
  identification. <P />(4 data files).

Title: Double Catastrophe of Coronal Flux Rope in Quadrupolar
    Magnetic Field
Authors: Zhang, Y. Z.; Hu, Y. Q.; Wang, J. X.
Bibcode: 2005ApJ...626.1096Z
Altcode:
  Using a relaxation method based on time-dependent ideal
  magnetohydrodynamic simulations, we find 2.5-dimensional force-free
  field solutions in spherical geometry, which are associated with an
  isolated flux rope embedded in a quadrupolar background magnetic
  field. The background field is of Antiochos type, consisting of a
  dipolar and an octopolar component with a neutral point somewhere in
  the equatorial plane. The flux rope is characterized by its magnetic
  fluxes, including the annular flux Φ<SUB>p</SUB> and the axial
  magnetic flux Φ<SUB>ϕ</SUB>, and its geometric features described
  by the height of the rope axis and the length of the vertical current
  sheet below the rope. It is found that for a given Φ<SUB>p</SUB>, the
  force-free field exhibits a complex catastrophic behavior with respect
  to increasing Φ<SUB>ϕ</SUB>. There exist two catastrophic points,
  and the catastrophic amplitude, measured by the jump in the height
  of the rope axis, is finite for both catastrophes. As a result, the
  flux rope may levitate stably in the corona after catastrophe, with a
  transverse current sheet above and a vertical current sheet below. The
  magnetic energy threshold for the two successive catastrophes are found
  to be larger than the corresponding partly open field energy. We argue
  that it is the transverse current sheet formed above the flux rope that
  provides a downward Lorentz force on the flux rope and thus keeps the
  rope levitating stably in the corona.

Title: Progress in solar dynamo theories
Authors: Jiang, Jie; Wang, Jing-Xiu
Bibcode: 2005PABei..23..121J
Altcode:
  The solar dynamo, which explains the origin and the evolution of
  all magnetic fields observed on the sun, is the fundamental and
  essential question of Solar Physics. Scientific inquiry into the
  question is more than an academic exercise. It is important to the
  development of space technology and the prediction of terrestrial
  climate. With the development of helioseismology, the solar dynamo
  has made great progresses. Staring from the observation, the paper
  summarizes some observations on the solar surface and the dynamic
  construction interior. The basic theories and the central models are
  introduced. Some unsolved problems are discussed.

Title: Two Extreme Double-peaked Line Emitters in the Sloan Digital
    Sky Survey
Authors: Wang, T. -G.; Dong, X. -B.; Zhang, X. -G.; Zhou, H. -Y.;
   Wang, J. -X.; Lu, Y. -J.
Bibcode: 2005ApJ...625L..35W
Altcode: 2005astro.ph..4320W
  Double-peaked Balmer lines have been observed in about 150 active
  galactic nuclei and were interpreted preferentially as emission from
  relativistic accretion disks. We report the discovery of extreme
  double-peaked lines in SDSS J0942+0900 and SDSS J1417+6141. The FWHM
  of the Hα line, ~=40,600 km s<SUP>-1</SUP>, in the first object is
  almost twice as large as the broadest previously known. By comparing
  the line profile with accretion disk models, we find that most of the
  line flux is emitted from a narrow annulus around 100r<SUB>g</SUB> in
  SDSS J0942+0900, and from a disk with radii between 100r<SUB>g</SUB>
  and 400r<SUB>g</SUB> in SDSS J1417+6141. This is the first time that
  an accretion disk at radii below 100r<SUB>g</SUB> has been directly
  probed through optical emission lines. A certain asymmetry in the
  disk is required for both objects. Another, much weaker, broad Hα
  component (W<SUB>λ</SUB>~20 Å and FWHM ~4000 km s<SUP>-1</SUP>) is
  also detected in both objects. Both objects show weak radio emission
  and strong high-ionization narrow lines.

Title: VizieR Online Data Catalog: Photometric redshifts of X-ray
    sources in CDF-S (Zheng+, 2004)
Authors: Zheng, W.; Mikles, V. J.; Mainieri, V.; Hasinger, G.; Rosati,
   P.; Wolf, C.; Norman, C.; Szokoly, G.; Gilli, R.; Tozzi, P.; Wang,
   J. X.; Zirm, A.; Giacconi, R.
Bibcode: 2005yCat..21550073Z
Altcode:
  Based on the photometry of 10 near-ultraviolet, optical, and
  near-infrared bands of the Chandra Deep Field-South, we estimate the
  photometric redshifts for 342 X-ray sources, which constitute ~99%
  of all the detected X-ray sources in the field. <P />(1 data file).

Title: Correlation Heights of the Sources of Solar Ultraviolet
    Emission Lines in a Quiet-Sun Region
Authors: Tu, Chuan-Yi; Zhou, Cheng; Marsch, Eckart; Wilhelm, Klaus;
   Zhao, Liang; Xia, Li-Dong; Wang, Jing-Xiu
Bibcode: 2005ApJ...624L.133T
Altcode:
  The radiance and Doppler-velocity maps of the emission lines of Si
  II, C IV, and Ne VIII obtained in a quiet region of the Sun by SUMER
  (Solar Ultraviolet Measurements of Emitted Radiation) are correlated
  with the vertical component, B<SUB>z</SUB>, of the magnetic field
  vector as extrapolated, by means of a force-free field model, from
  the photospheric magnetic field measured by MDI (Michelson Doppler
  Imager). It is found that, with increasing vertical height, each of the
  correlation coefficients initially increases to a maximum value before
  it decreases again. The height corresponding to this maximum is called
  the correlation height. For the data sets selected from a quiet-Sun
  region, the correlation heights of Si II and C IV are near 2 Mm,
  and for Ne VIII near 4 Mm. At their correlation heights, the averaged
  square root of the radiance of the emission lines of Si II and C IV,
  considered as a proxy of the plasma density, has a linear relationship
  with B<SUB>z</SUB>. This result supports the empirical concept that the
  solar transition region is very thin and still affected by frozen-in
  convection. A way for improvement of such studies is also outlined.

Title: Solar Wind Origin in Coronal Funnels
Authors: Tu, Chuan-Yi; Zhou, Cheng; Marsch, Eckart; Xia, Li-Dong;
   Zhao, Liang; Wang, Jing-Xiu; Wilhelm, Klaus
Bibcode: 2005Sci...308..519T
Altcode:
  The origin of the solar wind in solar coronal holes has long been
  unclear. We establish that the solar wind starts flowing out of the
  corona at heights above the photosphere between 5 megameters and 20
  megameters in magnetic funnels. This result is obtained by a correlation
  of the Doppler-velocity and radiance maps of spectral lines emitted
  by various ions with the force-free magnetic field as extrapolated
  from photospheric magnetograms to different altitudes. Specifically,
  we find that Ne<SUP>7+</SUP> ions mostly radiate around 20 megameters,
  where they have outflow speeds of about 10 kilometers per second,
  whereas C<SUP>3+</SUP> ions with no average flow speed mainly radiate
  around 5 megameters. Based on these results, a model for understanding
  the solar wind origin is suggested.

Title: An Overdensity of Lyα Emitters at Redshift z~5.7 near the
    Hubble Ultra Deep Field
Authors: Wang, J. X.; Malhotra, S.; Rhoads, J. E.
Bibcode: 2005ApJ...622L..77W
Altcode: 2005astro.ph..1479W
  We have identified an obvious and strong large-scale structure at
  redshift z~5.75 in a wide (31<SUP>'</SUP>×33<SUP>'</SUP>) field,
  narrowband survey of the Chandra Deep Field-South region. This structure
  is traced by 17 candidate Lyα emitters, among which 12 are found in an
  823 nm filter (corresponding to Lyα at z=5.77+/-0.03) and five in an
  815 nm image (z=5.70+/-0.03). The Lyα emitters in both redshift bins
  are concentrated in one quadrant of the field. The Hubble Ultra Deep
  Field, the Chandra Deep Field-South, and the Great Observatories Origins
  Deep Survey-South fields all lie near the edge of this overdensity
  region. Our results are consistent with reports of an overdensity in
  the Ultra Deep Field region at z~5.9. This structure is the highest
  redshift overdensity found so far.

Title: Strong Ca II Absorption Lines in the Reddened Quasar SDSS
J2339-0912: Evidence of the Collision/Merger in the Host Galaxy?
Authors: Wang, T. G.; Dong, X. B.; Zhou, H. Y.; Wang, J. X.
Bibcode: 2005ApJ...622L.101W
Altcode: 2005astro.ph..4319W
  We report the detection of strong Ca II/Mg II absorption lines
  at the quasar redshift in the narrow-line quasar SDSS J2339-0912
  (z=0.6604). The quasar exhibits strong Fe II, a small Balmer emission
  line width, and a very red B-K<SUB>s</SUB> color. Both the optical
  continuum and broad emission lines are reddened by SMC-like dust of
  E(B-V)~=1.0 mag, while its near-infrared color (J-K<SUB>s</SUB>=1.60)
  shows little reddening. The Ca II absorption lines are saturated and
  resolved with an FWHM of 362 km s<SUP>-1</SUP> and an equivalent width
  of W<SUB>CaIIK</SUB>=4.2 Å (in the source rest frame). Mg II absorption
  lines are also saturated and have a similar line width. The line profile
  and the fact that there is no evidence of starlight from the host galaxy
  suggest that these absorption lines are not of a stellar origin. The
  ratio of column density of Ca II to that of dust is consistent with
  that of the interstellar medium (ISM) in our Galaxy. We suggest that
  both the heavy reddening and the large absorption line width are due
  to the highly disturbed ISM on the line of sight toward the quasar and
  that the disturbance is caused by a galaxy collision or even merger
  in the quasar host galaxy.

Title: Cross-correlations between CMEs and other Solar Activity
    Indices
Authors: Song, W. B.; Wang, J. X.
Bibcode: 2005IAUS..226..213S
Altcode:
  Using the list of CMEs observed by SOHO/LASCO, we compile a daily CME
  counts from January 1996 to December 2003. Cross-correlations between
  the CME counts and other three solar activity indices, i.e., flare
  index, sunspot number, and photospheric magnetic flux, are examined
  in both real and Fourier spaces. We find that correlations are all
  significant in real space, but only photospheric magnetic flux has
  good correlation with CME counts in Fourier space. Typical periods of
  CME occurrence are presented and discussed.

Title: CMEs and Flux Appearance in the Periphery of Two Unipolar
    Sunspots
Authors: Yang, X. L.; Song, W. B.; Zhou, G. P.; Zhang, J.; Wang, J. X.
Bibcode: 2005IAUS..226..215Y
Altcode:
  A class of large-scale magnetic compositions have been identified to
  be CME-prolific, which is characterized by a huge unipolar sunspot
  appearing in a large-scale extended bipolar region in synoptic
  magnetic charts. To understand the CMEs' origin and the nature of flux
  appearance, we scrutinize the long time-sequence of MDI magnetograms
  of high-resolution mode for super active region AR9236. Two types of
  magnetic features are clearly identified. They are moving magnetic
  features (MMFs) emanated radially from the penumbral boundary and
  emerging flux regions (EFRs) whose growing opposite polarities rotate
  out from the inner boundary of sunspot moat along helical paths
  in opposite directions. The interaction between the MMFs and EFRs
  often creates multi-fold magnetic neutral lines where the flare/CMEs
  initiated.

Title: The north-south asymmetry of solar photospheric magnetic flux
Authors: Song, W. B.; Wang, J. X.; Ma, X.
Bibcode: 2005AcASn..46...19S
Altcode:
  The north-south asymmetry of solar photospheric magnetic flux is studied
  during years 1978-2002, finding that it has been relative to the solar
  activity cycle and peaked about the time of solar minimum. The dominance
  of solar activity has started to shift during the solar maximum from
  the northern hemisphere to the southern one. And its periodicities
  have been also discussed in detail with the wavelet transform.

Title: Wavelet analysis of photospheric magnetic flux
Authors: Song, W. B.; Wang, J. X.
Bibcode: 2005AdSpR..35..341S
Altcode:
  We link 342 NSO/Kitt Peak synoptic charts during 1978 to 2003 one by
  one in time order and reconstruct a daily sequence of photospheric
  magnetic flux (PMF). By using wavelet transform (WT) some typical
  mid-term periodicities of PMF are identified, such as 1.38-year,
  332-, 275- and 158-day periods. We discuss briefly their temporal
  evolutions and mutual relations in this paper. For a comparison with
  another solar general index, we also analyze the periodicities of total
  solar irradiance (TSI) with the same method. We find the wavelet power
  spectra of such two sequences are very similar. Therefore, we think
  PMF and TSI may have some common physical origins.

Title: The Chandra Deep Field-South: Optical Spectroscopy.  I.
Authors: Szokoly, G. P.; Bergeron, J.; Hasinger, G.; Lehmann, I.;
   Kewley, L.; Mainieri, V.; Nonino, M.; Rosati, P.; Giacconi, R.; Gilli,
   R.; Gilmozzi, R.; Norman, C.; Romaniello, M.; Schreier, E.; Tozzi,
   P.; Wang, J. X.; Zheng, W.; Zirm, A.
Bibcode: 2004ApJS..155..271S
Altcode: 2003astro.ph.12324S
  We present the results of our spectroscopic follow-up program of the
  X-ray sources detected in the 942 ks exposure of the Chandra Deep
  Field-South (CDFS). A total of 288 possible counterparts were observed
  at the VLT with the FORS1/FORS2 spectrographs for 251 of the 349 Chandra
  sources (including three additional faint X-ray sources). Spectra and
  R-band images are shown for all the observed sources and R-K colors are
  given for most of them. Spectroscopic redshifts were obtained for 168
  X-ray sources, of which 137 have both reliable optical identification
  and redshift estimate (including 16 external identifications). The
  R&lt;24 observed sample comprises 161 X-ray objects (181 optical
  counterparts), and 126 of them have unambiguous spectroscopic
  identification. There are two spikes in the redshift distribution,
  predominantly populated by type 2 active galactic nuclei (AGNs)
  but also type 1 AGN and X-ray normal galaxies: the one at z=0.734 is
  fairly narrow (in redshift space) and comprises two clusters/groups
  of galaxies centered on extended X-ray sources, the second one at
  z=0.674 is broader and should trace a sheetlike structure. The type
  1 and type 2 populations are clearly separated in X-ray/optical
  diagnostics involving parameters sensitive to absorption/reddening:
  X-ray hardness ratio (HR), optical/near-IR color, soft X-ray flux,
  and optical brightness. Nevertheless, these two populations cover
  similar ranges of hard X-ray luminosity and absolute K magnitude,
  thus trace similar levels of gravitational accretion. Consequently, we
  introduce a new classification based solely on X-ray properties, HR,
  and X-ray luminosity, consistent with the unified AGN model. This
  X-ray classification uncovers a large fraction of optically
  obscured, X-ray-luminous AGNs missed by the classical optical
  classification. We find a similar number of X-ray type 1 and type 2
  QSOs [L<SUB>X</SUB>(0.5-10keV)&gt;10<SUP>44</SUP> ergs s<SUP>-1</SUP>]
  at z&gt;2 (13 sources with unambiguous spectroscopic identification);
  most X-ray type 1 QSOs are bright, R&lt;~24, whereas most X-ray type
  2 QSOs have R&gt;~24, which may explain the difference with the CDFN
  results as few spectroscopic redshifts were obtained for R&gt;24 CDFN
  X-ray counterparts. There are X-ray type 1 QSOs down to z~0.5, but
  a strong decrease at z&lt;2 in the fraction of luminous X-ray type 2
  QSOs may indicate a cosmic evolution of the X-ray luminosity function
  of the type 2 population. An X-ray spectral analysis is required to
  confirm this possible evolution. The red color of most X-ray type 2
  AGNs could be due to dust associated with the X-ray absorbing material
  and/or a substantial contribution of the host galaxy light. The latter
  can also be important for some redder X-ray type 1 AGNs. There is
  a large population of EROs (R-K&gt;5) as X-ray counterparts, and
  their fraction strongly increases with decreasing optical flux, up
  to 25% for the R&gt;=24 sample. They cover the whole range of X-ray
  hardness ratios, comprise objects of various classes (in particular
  a high fraction of z&gt;~1 X-ray absorbed AGNs, but also elliptical
  and starburst galaxies) and more than half of them should be fairly
  bright X-ray sources [L<SUB>X</SUB>(0.5-10keV)&gt;10<SUP>42</SUP> ergs
  s<SUP>-1</SUP>]. Photometric redshifts will be necessary to derive
  the properties and evolution of the X-ray selected EROs. <P />Based
  on observations collected at the European Southern Observatory, Chile
  [ESO no. 66.A-0270(A) and 67.A-0418(A)].

Title: Low frequency radio signatures of coronal mass ejections
Authors: Wen, Ya-Yuan; Wang, Jing-Xiu
Bibcode: 2004PABei..22..284W
Altcode:
  Coronal mass ejections (CMEs) are the most spectacular phenomena
  of solar activities, and the solar events with the largest spatial
  scale. CMEs are often accompanied with other solar activities. Many
  solar phenomena are believed to have direct or indirect correlations
  with CMEs, such as solar flares, prominence eruption, helmet streamers,
  high-speed solar winds, coronal and interplanetary shock waves,
  and so on. Radio observations are an important complementary tool
  to study CMEs. Multi-frequency radio measurements not only study
  the initiation of CMEs, but also get more information on triggering
  mechanism of CMEs. In the present paper, we summarize the relationships
  between CMEs and low frequency radio bursts with the observational
  instruments and the radio signatures of CMEs being introduced
  and analyzed. The initiation mechanism and some open questions are
  discussed as well. Finally we claim that studies of CMEs must base on
  the multi-species data in all electromagnetic radiation wavelengths.

Title: Photometric Redshift of X-Ray Sources in the Chandra Deep
    Field-South
Authors: Zheng, W.; Mikles, V. J.; Mainieri, V.; Hasinger, G.; Rosati,
   P.; Wolf, C.; Norman, C.; Szokoly, G.; Gilli, R.; Tozzi, P.; Wang,
   J. X.; Zirm, A.; Giacconi, R.
Bibcode: 2004ApJS..155...73Z
Altcode: 2004astro.ph..6482Z
  Based on the photometry of 10 near-ultraviolet, optical, and
  near-infrared bands of the Chandra Deep Field-South, we estimate the
  photometric redshifts for 342 X-ray sources, which constitute ~99%
  of all the detected X-ray sources in the field. The models of spectral
  energy distribution are based on galaxies and a combination of power-law
  continuum and emission lines. Color information is useful for source
  classifications: type I active galactic nuclei (AGNs) show nonthermal
  spectral features that are distinct from galaxies and type II AGNs. The
  hardness ratio in X-ray and the X-ray-to-optical flux ratio are also
  useful discriminators. Using rudimentary color separation techniques, we
  are able to further refine our photometric redshift estimations. Among
  these sources, 173 have reliable spectroscopic redshifts, which we use
  to verify the accuracy of photometric redshifts and to modify the model
  inputs. The average relative dispersion in redshift distribution is ~8%,
  among the most accurate for photometric surveys. The high reliability
  of our results is attributable to the high quality and broad coverage
  of data as well as the applications of several independent methods and
  a careful evaluation of every source. We apply our redshift estimations
  to study the effect of redshift on broadband colors and to study the
  redshift distribution of AGNs. Our results show that both the hardness
  ratio and U-K color decline with redshift, which may be the result
  of a K-correction. The number of type II AGNs declines significantly
  at z&gt;2 and that of galaxies declines at z&gt;1. However, the
  distribution of type I AGNs exhibits less redshift dependence. As
  well, we observe a significant peak in the redshift distribution at
  z=0.6. We demonstrate that our photometric redshift estimation produces
  a reliable database for the study of X-ray luminosity of galaxies and
  AGNs. <P />Based on observations performed at the European Southern
  Observatory and observations with the NASA/ESA Hubble Space Telescope,
  obtained at the Space Telescope Science Institute, which is operated
  by the Association of Universities of Research in Astronomy, Inc.,
  under NASA contract NAS5-26555.

Title: Double-Power-Law Energy Spectra of Electrons from Solar
    <SUP>3</SUP>He-rich Events
Authors: Zhang, T. X.; Wang, J. X.
Bibcode: 2004ApJ...613L.165Z
Altcode:
  A possible explanation is proposed for the double-power-law energy
  spectrum of electrons from solar <SUP>3</SUP>He-rich events. According
  to the two-stage acceleration model that was developed by Zhang
  for the heating and acceleration of ions and electrons in solar
  <SUP>3</SUP>He-rich events, the energy spectrum of electrons in
  the thermal to power law energy range is derived. It is shown that
  the electron flux generally includes a thermal component at low
  energies and a nonthermal component with a power-law spectrum at high
  energies. To have the double-power-law energy spectrum of electrons
  at the high energies, three empirical models are proposed in terms of
  the dependences of the spectral power index, the electron temperature,
  and the threshold energy on the electron energy. The numerical result
  obtained by this study for the energy spectrum of electrons at energies
  ~1-200 keV fits very well with the double-power-law spectrum measurement
  given by Reames, von Rosenvinge, &amp; Lin.

Title: Identifying High-Redshift Active Galactic Nuclei Using X-Ray
    Hardness
Authors: Wang, J. X.; Malhotra, S.; Rhoads, J. E.; Norman, C. A.
Bibcode: 2004ApJ...612L.109W
Altcode: 2004astro.ph..5499W
  The X-ray color (hardness ratio) of optically undetected X-ray sources
  can be used to distinguish obscured active galactic nuclei (AGNs) at
  low and intermediate redshift from viable high-redshift (i.e., z&gt;5)
  AGN candidates. This will help determine the space density, ionizing
  photon production, and X-ray background contribution of the earliest
  detectable AGNs. High-redshift AGNs should appear soft in X-rays,
  with hardness ratio HR~-0.5, even if there is strong absorption
  by a hydrogen column density N<SUB>H</SUB> up to 10<SUP>23</SUP>
  cm<SUP>-2</SUP>, simply because the absorption redshifts out of the
  soft X-ray band in the observed frame. Here the X-ray hardness ratio
  is defined as HR=(H-S)/(H+S), where S and H are the soft and hard band
  net counts detected by Chandra. High-redshift AGNs that are Compton
  thick (N<SUB>H</SUB>&gt;~10<SUP>24</SUP> cm<SUP>-2</SUP>) could have
  HR~0.0 at z&gt; 5. However, these should be rare in deep Chandra
  images, since they have to be &gt;~10 times brighter intrinsically,
  which implies a &gt;~100 times drop in their space density. Applying
  the hardness criterion (HR&lt;0.0) can filter out about 50% of the
  candidate high-redshift AGNs selected from deep Chandra images.

Title: X-Ray Nondetection of the Lyα Emitters at z~4.5
Authors: Wang, J. X.; Rhoads, J. E.; Malhotra, S.; Dawson, S.; Stern,
   D.; Dey, A.; Heckman, T. M.; Norman, C. A.; Spinrad, H.
Bibcode: 2004ApJ...608L..21W
Altcode: 2004astro.ph..4611W
  The Lyα emitters found at z~4.5 by the Large Area Lyman Alpha (LALA)
  survey have high equivalent widths in the Lyα line, which can be
  produced by either narrow-lined active galactic nuclei (AGNs) or by
  stellar populations with a very high proportion of young, massive
  stars. To investigate the AGN scenario, we obtained two deep Chandra
  exposures to study the X-ray nature of the Lyα emitters. The 172
  ks deep Chandra image on the LALA Boötes field was presented in
  a previous paper, and in this Letter we present a new Chandra deep
  exposure (174 ks) on the LALA Cetus field, which doubled our sample of
  X-ray-imaged Lyα sources and imaged the brightest source among our Lyα
  emitters. None of the 101 Lyα sources covered by two Chandra exposures
  were detected individually in X-rays, with a 3 σ limiting X-ray flux of
  F<SUB>0.5-10.0keV</SUB>&lt;3.3×10<SUP>-16</SUP> ergs cm<SUP>-2</SUP>
  s<SUP>-1</SUP> for on-axis targets. The sources remain undetectable
  in the stacked image, implying a 3 σ limit to the average luminosity
  of L<SUB>2-8keV</SUB>&lt;2.8×10<SUP>42</SUP> ergs s<SUP>-1</SUP>. The
  resulting X-ray to Lyα ratio is greater than 21 times lower than the
  ratios for known high-redshift type II quasars. Together with optical
  spectra obtained at Keck, we conclude that no evidence of AGN activity
  was found among our Lyα emitters at z~4.5.

Title: Deep Chandra image in the Bootes Field
Authors: Wang, J. X.; Malhotra, S.; Rhoads, J. E.; Brown, M. J. I.;
   Dey, A.; Jannuzi, B. T.; Dawson, S.; Spinrad, H.; Heckman, T. M.;
   Norman, C. A.; Stern, D.; Tiede, G. P.; Tozzi, P.
Bibcode: 2004AAS...204.4814W
Altcode: 2004BAAS...36..748W
  A 172 ks long Chandra exposure was carried out in the LALA-Bootes field
  and a similar one for the LALA cetus field. These exposure were deep
  enough to detect LALA sources, if they were type-II quasars. Lyman-alpha
  emitters found with LALA show high equivalent widths and AGN phenomenon
  is one explanation. A total of 101 Ly-alpha emitters are covered by the
  two Chandra images. No Ly-alpha emitters are detected individually or
  in the co-added X-ray images. Our analysis indicates that fewer than
  4.8 Ly-alpha emitters could be possible AGNs based on the upper limit
  of their average X-ray to Ly-alpha ratio. The two X-ray images are
  among the deepest taken by Chandra, with a total of 348 X-ray sources
  detected, similar to the number of X-ray sources in Chandra Deep Field
  South. We also see field-to-field variations of the hard X-ray source
  counts in different Chandra fields, due to large scale structure.

Title: Lyman Alpha Galaxies at High Redshift
Authors: Rhoads, J. E.; Malhotra, S.; Dawson, S.; Dey, A.; Jannuzi,
   B. T.; Spinrad, H.; Stern, D.; Wang, J. X.; Xu, C.; Brown, M. J. I.;
   Landes, E.
Bibcode: 2004AAS...204.4803R
Altcode: 2004BAAS...36..746R
  Because strong Lyman alpha emission is expected from young star
  forming galaxies at high redshift, it offers an efficient tool for
  identifying these galaxies. The Large Area Lyman Alpha survey is one
  of the first and largest successful searches for Lyman alpha emitting
  galaxies at high redshift. In the LALA Bootes field (which lies within
  the NOAO Deep Wide-Field Survey's Bootes field) we have obtained deep
  narrowband images covering 1/3 square degree in each of eight filters,
  sampling redshifts z=4.5, 5.7, and 6.5. We focus here on the higher
  redshift windows, where we have confirmed a luminous Lyman alpha
  emitting galaxy at z=6.535 and several others in the z=5.7 window. We
  discuss the physical properties of these objects, including their
  contribution to star formation rates and metal production. We also
  discuss the implications of Lyman alpha galaxy observations at z=6.5
  for reionization.

Title: Identifying high redshift AGNs from X-ray colors
Authors: Wang, J. X.; Rhoads, J. E.; Malhotra, S.; Norman, C. A.
Bibcode: 2004AAS...204.4407W
Altcode: 2004BAAS...36Q.732W
  The X-ray color (hardness ratio) can be used to select high redshift
  active galactic nuclei (AGNs) among the x-ray selected, optically
  blank candidates. High redshift AGNs should appear soft in X-ray with
  hardness ratio HR ∼ -0.5, even if there is strong absorption with
  N<SUB>H</SUB> up to 10<SUP>23</SUP> cm<SUP>-2</SUP>, simply because
  the absorption redshifts out of the soft X-ray band in the observed
  frame. Here the X-ray hardness ratio is defined as HR= (H-S)/(H+S),
  where S and H are the soft and hard band net counts detected by
  Chandra. High redshift AGNs that are Compton thick (N<SUB>H</SUB> &gt;=
  10<SUP>24</SUP> cm<SUP>-2</SUP>) could have HR ∼ 0.0, however, these
  should be rare in deep Chandra images, since they have to be ∼ 10
  times brighter intrinsicly, which leads to ∼ 100 times drop in their
  space density. All known z &gt; 4 AGNs show soft x-ray colors. Applying
  the hardness criterion (HR &lt; 0.0) can filter out about 50% of the
  candidate high redshift AGNs selected from deep Chandra images.

Title: Investigation for the cosmic ray ground level enhancements
    during solar cycle 23
Authors: Wang, R. G.; Wang, J. X.
Bibcode: 2004cosp...35.2410W
Altcode: 2004cosp.meet.2410W
  Major solar energetic particle (SEP) events associated with large
  solar flares can give rise to the cosmic ray ground level enhancements
  (GLEs). Up to December 2003 during solar activity cycle 23, 12 GLEs
  (Number from 55 to 66) have been recorded by the worldwide network
  of neutron monitors (NMs) in the 87 solar proton events (with peak
  flux exceeding 10 {(cm^2 sec ster)}<SUP>-1</SUP> for more than 10
  MeV solar protons ). Eeight of the 12 GLEs (67%) are originated from
  southern hemisphere and 10 of the 12 GLEs (83%) are originated from
  western hemisphere. Each GLE is corresponded by a solar coronal mass
  ejection (CME) which had the potential of producing disturbances to the
  geospace. Among the 12 relevant CMEs 8 large ones should be responsible
  for the 8 major geomagnetic storms (defined by disturbance storm time
  index ≤ -100 nT). The largest 3 geomagnetic storms (Dst≤ -300 nT)
  correspond to the 3 GLEs (No.59, No.65 and No.66) which have great
  proton flux with energy &gt; 10 MeV. It seems to imply that the solar
  proton events having great proton flux are more likely to bring major
  geomagnetic storms. Furthermore, solar proton event with high flux is
  not a condition for creating GLE. Some proposal factors are discussed
  for GLE production.

Title: The 172 ks Chandra Exposure of the LALA Bootes Field: X-Ray
    Source Catalog
Authors: Wang, J. X.; Malhotra, S.; Rhoads, J. E.; Brown, M. J. I.;
   Dey, A.; Heckman, T. M.; Jannuzi, B. T.; Norman, C. A.; Tiede, G. P.;
   Tozzi, P.
Bibcode: 2004AJ....127..213W
Altcode: 2003astro.ph..9705W
  We present an analysis of a deep, 172 ks Chandra observation of
  the Large Area Lyman Alpha survey (LALA) Bootes field, obtained
  with the Advanced CCD Imaging Spectrometer (ACIS-I) on board the
  Chandra X-Ray Observatory. This is one of the deepest Chandra images
  of the extragalactic sky; only the 2 Ms Chandra Deep Field North
  (CDF-N) and 1 Ms Chandra Deep Field South (CDF-S) are substantially
  deeper. In this paper we present the X-ray source catalog obtained
  from this image, along with an analysis of source counts and optical
  identifications. The X-ray image is composed of two individual
  observations obtained in 2002 and reaches 0.5-2.0 and 2.0-10.0 keV
  flux limits of 1.5×10<SUP>-16</SUP> and 1.0×10<SUP>-15</SUP> ergs
  cm<SUP>-2</SUP> s<SUP>-1</SUP>, respectively, for point sources near
  the aim point. A total of 168 X-ray sources were detected: 160 in the
  0.5-7.0 keV band, 132 in the 0.5-2.0 keV band, and 111 in the 2.0-7.0
  keV band. The X-ray source counts were derived and compared with those
  from other Chandra deep surveys; the hard X-ray source density of the
  LALA Bootes field is 33% higher than that of CDF-S at the flux level of
  2.0×10<SUP>-15</SUP> ergs cm<SUP>-2</SUP> s<SUP>-1</SUP>, confirming
  the field-to-field variances of the hard-band source counts reported by
  previous studies. The deep exposure resolves &gt;~72% of the 2.0-10.0
  keV X-ray background. Our primary optical data are R-band imaging from
  the NOAO Deep Wide-Field Survey (NDWFS), with a limiting magnitude of
  R=25.7 (Vega, 3 σ, and 4" diameter aperture). We have found optical
  counterparts for 152 of the 168 Chandra sources (90%); 144 of these
  are detected in the R-band image, and eight have optical counterparts
  in other bands (either B<SUB>W</SUB>, V, I, or z'). Among the R-band
  nondetected sources, not more than 11 of them can possibly be at z&gt;5,
  based on the hardness ratios of their X-ray emission and nondetections
  in bluer bands (B<SUB>W</SUB>, V). The majority (~76%) of the X-ray
  sources are found to have log(f<SUB>X</SUB>/f<SUB>R</SUB>) within
  0.0+/-1 these are believed to be AGNs. Most of the X-ray-faint/optically
  bright sources [log(f<SUB>X</SUB>/f<SUB>R</SUB>)&lt;-1.0] are optically
  extended; these are low-z normal galaxies or low-luminosity AGNs. There
  is also a population of sources that are X-ray overluminous for their
  optical magnitudes [log(f<SUB>X</SUB>/f<SUB>R</SUB>)&gt;1.0], which
  are harder in X-ray and are probably obscured AGNs.

Title: Reconnection in the lower solar atmosphere and coronal mass
    ejections
Authors: Wang, J. X.
Bibcode: 2004cosp...35.3644W
Altcode: 2004cosp.meet.3644W
  In 1985 a phenomenon in solar physics, named as magnetic flux
  cancellation, was first described in details by Livi, Wang, Martin
  (1995). Since then, it has been revealed that flux cancellation is
  intrinsically correlated to the most, if not all, types of solar
  activity, such as flare, filament formation and eruption in active
  regions, and ubiquitous small-scale activity, e.g., X-ray bright
  points, explosive events, mini-filament eruptions and so on. Only
  recently, it was discovered that flux cancellation appeared to be
  a very key magnetic evolution leading to the initiation of coronal
  mass ejections (Zhang et al. 2001; Zhang and Wang, 2001; Zhang, Wang,
  Nitta, 2001). On the other hand, the nature of flux cancellation has
  become a topic of persistent interests and debates. In this talk,
  we review the observational properties of magnetic flux cancellation
  and the relevant theoretical studies, and present observations of
  flux cancellation from vector magnetograph in CME associated source
  regions. Then, we demonstrate that at least some well-observed flux
  cancellation by vector magnetograph fits nicely the scenario of magnetic
  reconnection in the lower solar atmosphere, i.e., the partially ionized
  plasma. It is suggested that the magnetic reconnection in the lower
  solar atmosphere is the key elements in the CME magnetism.

Title: Periodicities in solar coronal mass ejections
Authors: Lou, Yu-Qing; Wang, Yu-Ming; Fan, Zuhui; Wang, Shui; Wang,
   Jing Xiu
Bibcode: 2003MNRAS.345..809L
Altcode: 2003astro.ph..7277L
  Mid-term quasi-periodicities in solar coronal mass ejections (CMEs)
  during the most recent solar maximum cycle 23 are reported here for the
  first time using the four-year data (1999 February 5 to 2003 February
  10) of the Large Angle Spectrometric Coronagraph on board the Solar and
  Heliospheric Observatory. In parallel, mid-term quasi-periodicities in
  solar X-ray flares (class &gt;M5.0) from the Geosynchronous Operational
  Environment Satellites and in daily averages of Ap index for geomagnetic
  disturbances from the World Data Center at the International Association
  for Geomagnetism and Aeronomy are also examined for the same four-year
  time-span. By Fourier power spectral analyses, the CME data appear
  to contain significant power peaks at periods of ~358 +/- 38, ~272
  +/- 26, ~196 +/- 13 d and so forth, while, except for the ~259 +/-
  24 d period, X-ray solar flares of class &gt;~M5.0 show the familiar
  Rieger-type quasi-periods at ~157 +/- 11, ~122 +/- 5, ~98 +/- 3 d and
  shorter ones down to ~34 +/- 0.5 d. In the data of daily averages of Ap
  index, the two significant peaks at periods ~273 +/- 26 and ~187 +/-
  12 d (the latter is most prominent) could imply that CMEs (periods
  at ~272 +/- 26 and ~196 +/- 13 d) may be proportionally correlated
  with quasi-periodic geomagnetic storm disturbances. At the speculative
  level, the ~138 +/- 6 d period might imply that X-ray flares of class
  &gt;~M5.0 (period at ~157 +/- 11 d) drive certain types of geomagnetic
  disturbances; the ~28 +/- 0.2 d periodicity is most likely caused by
  recurrent high-speed solar winds at the Earth's magnetosphere. For
  the same three data sets, we further perform Morlet wavelet analysis
  to derive period-time contours and identify wavelet power peaks and
  time-scales at the 99 per cent confidence level for comparisons. Several
  conceptual aspects of possible equatorially trapped Rossby-type waves
  at and beneath the solar photosphere are discussed.

Title: On the Latitudinal Distribution of Sunspot Groups over a
    Solar Cycle
Authors: Li, K. J.; Wang, J. X.; Zhan, L. S.; Yun, H. S.; Liang,
   H. F.; Zhao, H. J.; Gu, X. M.
Bibcode: 2003SoPh..215...99L
Altcode:
  The latitudinal distribution of sunspot groups over a solar cycle
  is investigated. Although individual sunspot groups of a solar cycle
  emerge randomly at any middle and low latitude, the whole latitudinal
  distribution of sunspot groups of the cycle is not stochastic and,
  in fact, can be represented by a probability density function of the
  Γ distribution having maximum probability at about 15.5°. The maximum
  amplitude of a solar cycle is found to be positively correlated against
  the number of sunspot groups at high latitude (≥35°) over the cycle,
  as well as the mean latitude. Also, the relation between the asymmetry
  of sunspot groups and its latitude is investigated, and a pattern of
  the N-S asymmetry in solar activity is suggested.

Title: A Fluid Dynamics Approach for the Computation of Nonlinear
    Force-Free Magnetic Field
Authors: Li, Jing-Qun; Wang, Jing-Xiu; Wei, Feng-Si
Bibcode: 2003ChJAA...3..247L
Altcode:
  Inspired by the analogy between the magnetic field and velocity field
  of incompressible fluid flow, we propose a fluid dynamics approach for
  computing nonlinear force-free magnetic fields. This method has the
  advantage that the divergence-free condition is automatically satisfied,
  which is a sticky issue for many other algorithms, and we can take
  advantage of modern high resolution algorithms to process the force-free
  magnetic field. Several tests have been made based on the well-known
  analytic solution proposed by Low &amp; Lou. The numerical results
  are in satisfactory agreement with the analytic ones. It is suggested
  that the newly proposed method is promising in extrapolating the active
  region or the whole sun magnetic fields in the solar atmosphere based
  on the observed vector magnetic field on the photosphere.

Title: An Explanation for Large Enhancements of Nitrogen relative
    to Carbon and Oxygen in Solar <SUP>3</SUP>He-rich Events
Authors: Zhang, T. X.; Wang, J. X.
Bibcode: 2003ApJ...588L..57Z
Altcode:
  Preferential heating and abundance enhancements of carbon (C),
  nitrogen (N), and oxygen (O) in solar <SUP>3</SUP>He-rich energetic
  particles are investigated in terms of the two-stage acceleration model
  proposed by Zhang. It is shown that C<SUP>+5</SUP>, N<SUP>+6</SUP>,
  and O<SUP>+7</SUP> are preferentially heated by H-cyclotron waves with a
  frequency close to twice the <SUP>3</SUP>He-cyclotron frequency through
  the third harmonic resonance. If the initial electron temperature of
  the solar corona is in the range of ~2-3.2 MK, the abundance of N in
  high-energy particles due to the second-stage acceleration is enhanced
  by a factor of ~4-12 relative to C and O. The abundance pattern of C,
  N, and O obtained from the two-stage acceleration model is consistent
  with recent measurements (Mason, Mazur, &amp; Dwyer). In addition,
  harmonic resonances of neon, silicon, magnesium, sulfur, calcium,
  and iron with the H-cyclotron waves are discussed.

Title: No X-Ray-bright Type II Quasars among the Lyα Emitters
Authors: Malhotra, S.; Wang, J. X.; Rhoads, J. E.; Heckman, T. M.;
   Norman, C. A.
Bibcode: 2003ApJ...585L..25M
Altcode: 2003astro.ph..1622M
  The Lyα emitters found at z=4.5 and 5.7 by the Large Area Lyman Alpha
  (LALA) survey have high equivalent widths in the Lyα line. Such lines
  can be produced by narrow-lined active galactic nuclei or by stellar
  populations with a very high proportion of young massive stars. To
  check for type II (i.e., narrow-lined) quasars, we obtained a deep
  X-ray image of 49 Lyα sources in a single field of the ACIS instrument
  on the Chandra X-Ray Observatory. None of these sources was detected
  with a 3 σ limiting X-ray luminosity of 2.9×10<SUP>43</SUP> ergs
  s<SUP>-1</SUP>. For comparison, the two known high-redshift type II
  quasars have luminosities of 4×10<SUP>43</SUP> ergs s<SUP>-1</SUP>
  before extinction correction. The sources remain undetected in
  stacked images of the 49 Lyα sources (with 6.5 Ms effective Chandra
  on-axis exposure) at 3 σ limits of 4.9×10<SUP>42</SUP>. The resulting
  X-ray-to-Lyα ratio is about 4-24 times lower than the ratio for known
  type II quasars, while the average Lyα luminosity of the LALA sample
  is between the two type II's. The cumulative X-ray-to-Lyα ratio limit
  is also below that of 90% of low-redshift Seyfert galaxies.

Title: Influence of turbulent magnetic fields on mode frequencies
Authors: Bi, S. L.; Liao, Y.; Wang, J. X.
Bibcode: 2003A&A...397.1069B
Altcode:
  To investigate the physical nature of solar convective zone, we employ
  the observed frequency shifts of solar oscillations to study the
  influence of magnetic perturbation inside the Sun on the low-l solar
  p-mode oscillations. We describe the various possibility of frequency
  shifts for a time-dependent source of MHD turbulence. For the magnetic
  perturbation contribution, we obtain the frequency shifts of modes with
  different degree as a function of the spectrum of fluctuating magnetic
  field. The frequency shift is found to increase with the strength of
  magnetic fields in solar interior, and its temporal behavior closely
  follows the phase of the synthetic solar activity cycle. Our analysis
  indicates that the magnetic activities cause shifts of up to 0.3 muHz
  . It is obviously shown that mode frequency, which is sensitive to
  the effect of magnetic fields, can be used as a diagnostic tool for
  the presence of turbulent magnetic fields in the convection zone.

Title: Direct Evidence for Neutrino Flavor Transformation from
    Neutral-Current Interactions in SNO
Authors: McDonald, A. B.; Ahmad, Q. R.; Allen, R. C.; Andersen, T. C.;
   Anglin, J. D.; Barton, J. C.; Beier, E. W.; Bercovitch, M.; Bigu, J.;
   Biller, S. D.; Black, R. A.; Blevis, I.; Boardman, R. J.; Boger, J.;
   Bonvin, E.; Boulay, M. G.; Bowler, M. G.; Bowles, T. J.; Brice, S. J.;
   Browne, M. C.; Bullard, T. V.; Bühler, G.; Cameron, J.; Chan, Y. D.;
   Chen, H. H.; Chen, M.; Chen, X.; Cleveland, B. T.; Clifford, E. T. H.;
   Cowan, J. H. M.; Cowen, D. F.; Cox, G. A.; Dai, X.; Dalnoki-Veress, F.;
   Davidson, W. F.; Doe, P. J.; Doucas, G.; Dragowsky, M. R.; Duba, C. A.;
   Duncan, F. A.; Dunford, M.; Dunmore, J. A.; Earle, E. D.; Elliott,
   S. R.; Evans, H. C.; Ewan, G. T.; Farine, J.; Fergani, H.; Ferraris,
   A. P.; Ford, R. J.; Formaggio, J. A.; Fowler, M. M.; Frame, K.; Frank,
   E. D.; Frati, W.; Gagnon, N.; Germani, J. V.; Gil, S.; Graham, K.;
   Grant, D. R.; Hahn, R. L.; Hallin, A. L.; Hallman, E. D.; Hamer,
   A. S.; Hamian, A. A.; Handler, W. B.; Haq, R. U.; Hargrove, C. K.;
   Harvey, P. J.; Hazama, R.; Heeger, K. M.; Heintzelman, W. J.; Heise,
   J.; Helmer, R. L.; Hepburn, J. D.; Heron, H.; Hewett, J.; Hime, A.;
   Howe, M.; Hykawy, J. G.; Isaac, M. C. P.; Jagam, P.; Jelley, N. A.;
   Jillings, C.; Jonkmans, G.; Kazkaz, K.; Keener, P. T.; Klein, J. R.;
   Knox, A. B.; Komar, R. J.; Kouzes, R.; Kutter, T.; Kyba, C. C. M.;
   Law, J.; Lawson, I. T.; Lay, M.; Lee, H. W.; Lesko, K. T.; Leslie,
   J. R.; Levine, I.; Locke, W.; Luoma, S.; Lyon, J.; Majerus, S.; Mak,
   H. B.; Maneira, J.; Manor, J.; Marino, A. D.; McCauley, N.; McDonald,
   D. S.; McFarlane, K.; McGregor, G.; Meijer Drees, R.; Mifflin, C.;
   Miller, G. G.; Milton, G.; Moffat, B. A.; Moorhead, M.; Nally, C. W.;
   Neubauer, M. S.; Newcomer, F. M.; Ng, H. S.; Noble, A. J.; Norman,
   E. B.; Novikov, V. M.; O'Neill, M.; Okada, C. E.; Ollerhead, R. W.;
   Omori, M.; Orrell, J. L.; Oser, S. M.; Poon, A. W. P.; Radcliffe,
   T. J.; Roberge, A.; Robertson, B. C.; Robertson, R. G. H.; Rosendahl,
   S. S. E.; Rowley, J. K.; Rusu, V. L.; Saettler, E.; Schaffer, K. K.;
   Schwendener, M. H.; Schülke, A.; Seifert, H.; Shatkay, M.; Simpson,
   J. J.; Sims, C. J.; Sinclair, D.; Skensved, P.; Smith, A. R.; Smith,
   M. W. E.; Spreitzer, T.; Starinsky, N.; Steiger, T. D.; Stokstad,
   R. G.; Stonehill, L. C.; Storey, R. S.; Sur, B.; Tafirout, R.; Tagg,
   N.; Tanner, N. W.; Taplin, R. K.; Thorman, M.; Thornewell, P. M.;
   Trent, P. T.; Tserkovnyak, Y. I.; van Berg, R.; van de Water, R. G.;
   Virtue, C. J.; Waltham, C. E.; Wang, J. -X.; Wark, D. L.; West,
   N.; Wilhelmy, J. B.; Wilkerson, J. F.; Wilson, J. R.; Wittich, P.;
   Wouters, J. M.; Yeh, M.
Bibcode: 2002AIPC..646...43M
Altcode:
  The Sudbury Neutrino Observatory (SNO) is a 1,000 tonne heavy
  water Cerenkov-based neutrino detector situated 2,000 meters
  underground in INCO's Creighton Mine near Sudbury, Ontario,
  Canada. For the neutrinos from <SUP>8</SUP>B decay in the Sun SNO
  observes the Charged Current neutrino reaction sensitive only
  to electron neutrinos and others (Neutral Current and Elastic
  Scattering) sensitive to all active neutrino types and thereby
  can search for direct evidence of neutrino flavor change. Using
  these reactions and assuming the standard <SUP>8</SUP>B shape, the
  ve component of the <SUP>8</SUP>B solar flux is φe = 1.76<SUB>-
  0.05</SUB><SUP>+0.05</SUP>(stat.)<SUB>- 0.09</SUB><SUP>+0.09</SUP>
  (syst.) × 10<SUP>6</SUP> cm<SUP>-2</SUP>s<SUP>-1</SUP> for a kinetic
  energy threshold of 5 MeV. The non-ve component is fgr μτ = 3.41<SUB>-
  0.45</SUB><SUP>+0.45</SUP>(stat.)<SUB>- 0.45</SUB><SUP>+0.48</SUP>
  (syst.) × 10<SUP>6</SUP> cm<SUP>-2</SUP>s<SUP>-1</SUP>, 5.3σ
  greater than zero, providing strong evidence for solar ve flavor
  transformation. The total flux measured with the NC reaction is
  fgr NC = 5.09<SUB>- 0.43</SUB><SUP>+0.44</SUP>(stat.)<SUB>-
  0.43</SUB><SUP>+0.46</SUP> (syst.) × 10<SUP>6</SUP>
  cm<SUP>-2</SUP>s<SUP>-1</SUP>, consistent with solar models. For charged
  current events, assuming an undistorted <SUP>8</SUP>B spectrum, the
  night minus day rate is 14.0% +/- 6.3%<SUB>-1.4</SUB><SUP>+1.5</SUP>% of
  the average rate. If the total flux of active neutrinos is additionally
  constrained to have no asymmetry, the ve asymmetry is found to be
  7.0% +/- 4.9%<SUB>-1.2</SUB><SUP>+1.3</SUP>%. A global solar neutrino
  analysis in terms of matter-enhanced oscillations of two active flavors
  strongly favors the Large Mixing Angle (LMA) solution.

Title: A statistical study on the geoeffectiveness of Earth-directed
    coronal mass ejections from March 1997 to December 2000
Authors: Wang, Y. M.; Ye, P. Z.; Wang, S.; Zhou, G. P.; Wang, J. X.
Bibcode: 2002JGRA..107.1340W
Altcode:
  We have identified 132 Earth-directed coronal mass ejections
  (CMEs) based on the observations of the Large Angle Spectroscopic
  Coronagraph (LASCO) and Extreme Ultraviolet Imaging Telescope (EIT)
  on board of Solar and Heliospheric Observatory (SOHO) from March
  1997 to December 2000 and carried out a statistical study on their
  geoeffectiveness. The following results are obtained: (1) Only 45%
  of the total 132 Earth-directed halo CMEs caused geomagnetic storms
  with Kp ≥ 5; (2) The initial sites of these geoeffective halo CMEs
  are rather symmetrically distributed in the heliographic latitude
  of the visible solar disc, while asymmetrical in longitude with the
  majority located in the west side of the central meridian; (3) The
  frontside halo CMEs accompanied with solar flares (identified from
  GOES-8 satellite observations) seem to be more geoeffective; (4) Only a
  weak correlation between the CME projected speed and the transit time
  is revealed. However, for the severe geomagnetic storms (with Kp ≥
  7), a significant correlation at the confidence level of 99% is found.

Title: A method for the prediction of relative sunspot number for
    the remainder of a progressing cycle with application to cycle 23
Authors: Li, K. J.; Zhan, L. S.; Wang, J. X.; Liu, X. H.; Yun, H. S.;
   Xiong, S. Y.; Liang, H. F.; Zhao, H. Z.
Bibcode: 2002A&A...392..301L
Altcode:
  In this paper, we investigate the prospect of using previously
  occurring sunspot cycle signatures to determine future behavior in
  an ongoing cycle, with specific application to cycle 23, the current
  sunspot cycle. We find that the gross level of solar activity (i.e.,
  the sum of the total number of sunspots over the course of a sunspot
  cycle) associated with cycle 23, based on a comparison of its first
  several years of activity against similar periods of preceding cycles,
  is such that cycle 23 best compares to cycle 2. Compared to cycles
  2 and 22, respectively, cycle 23 appears 1.08 times larger and 0.75
  times as large. Because cycle 2 was of shorter period, we infer that
  cycle 23 also might be of shorter length (period less than 11 years),
  ending sometime in late 2006 or early 2007.

Title: Direct Evidence for Neutrino Flavor Transformation from
    Neutral-Current Interactions in the Sudbury Neutrino Observatory
Authors: Ahmad, Q. R.; Allen, R. C.; Andersen, T. C.; Anglin, J. D.;
   Barton, J. C.; Beier, E. W.; Bercovitch, M.; Bigu, J.; Biller, S. D.;
   Black, R. A.; Blevis, I.; Boardman, R. J.; Boger, J.; Bonvin, E.;
   Boulay, M. G.; Bowler, M. G.; Bowles, T. J.; Brice, S. J.; Browne,
   M. C.; Bullard, T. V.; Bühler, G.; Cameron, J.; Chan, Y. D.; Chen,
   H. H.; Chen, M.; Chen, X.; Cleveland, B. T.; Clifford, E. T.; Cowan,
   J. H.; Cowen, D. F.; Cox, G. A.; Dai, X.; Dalnoki-Veress, F.; Davidson,
   W. F.; Doe, P. J.; Doucas, G.; Dragowsky, M. R.; Duba, C. A.; Duncan,
   F. A.; Dunford, M.; Dunmore, J. A.; Earle, E. D.; Elliott, S. R.;
   Evans, H. C.; Ewan, G. T.; Farine, J.; Fergani, H.; Ferraris, A. P.;
   Ford, R. J.; Formaggio, J. A.; Fowler, M. M.; Frame, K.; Frank, E. D.;
   Frati, W.; Gagnon, N.; Germani, J. V.; Gil, S.; Graham, K.; Grant,
   D. R.; Hahn, R. L.; Hallin, A. L.; Hallman, E. D.; Hamer, A. S.;
   Hamian, A. A.; Handler, W. B.; Haq, R. U.; Hargrove, C. K.; Harvey,
   P. J.; Hazama, R.; Heeger, K. M.; Heintzelman, W. J.; Heise, J.;
   Helmer, R. L.; Hepburn, J. D.; Heron, H.; Hewett, J.; Hime, A.; Howe,
   M.; Hykawy, J. G.; Isaac, M. C.; Jagam, P.; Jelley, N. A.; Jillings,
   C.; Jonkmans, G.; Kazkaz, K.; Keener, P. T.; Klein, J. R.; Knox, A. B.;
   Komar, R. J.; Kouzes, R.; Kutter, T.; Kyba, C. C.; Law, J.; Lawson,
   I. T.; Lay, M.; Lee, H. W.; Lesko, K. T.; Leslie, J. R.; Levine, I.;
   Locke, W.; Luoma, S.; Lyon, J.; Majerus, S.; Mak, H. B.; Maneira, J.;
   Manor, J.; Marino, A. D.; McCauley, N.; McDonald, A. B.; McDonald,
   D. S.; McFarlane, K.; McGregor, G.; Meijer Drees, R.; Mifflin,
   C.; Miller, G. G.; Milton, G.; Moffat, B. A.; Moorhead, M.; Nally,
   C. W.; Neubauer, M. S.; Newcomer, F. M.; Ng, H. S.; Noble, A. J.;
   Norman, E. B.; Novikov, V. M.; O'Neill, M.; Okada, C. E.; Ollerhead,
   R. W.; Omori, M.; Orrell, J. L.; Oser, S. M.; Poon, A. W.; Radcliffe,
   T. J.; Roberge, A.; Robertson, B. C.; Robertson, R. G.; Rosendahl,
   S. S.; Rowley, J. K.; Rusu, V. L.; Saettler, E.; Schaffer, K. K.;
   Schwendener, M. H.; Schülke, A.; Seifert, H.; Shatkay, M.; Simpson,
   J. J.; Sims, C. J.; Sinclair, D.; Skensved, P.; Smith, A. R.; Smith,
   M. W.; Spreitzer, T.; Starinsky, N.; Steiger, T. D.; Stokstad, R. G.;
   Stonehill, L. C.; Storey, R. S.; Sur, B.; Tafirout, R.; Tagg, N.;
   Tanner, N. W.; Taplin, R. K.; Thorman, M.; Thornewell, P. M.; Trent,
   P. T.; Tserkovnyak, Y. I.; van Berg, R.; van de Water, R. G.; Virtue,
   C. J.; Waltham, C. E.; Wang, J. -X.; Wark, D. L.; West, N.; Wilhelmy,
   J. B.; Wilkerson, J. F.; Wilson, J. R.; Wittich, P.; Wouters, J. M.;
   Yeh, M.
Bibcode: 2002PhRvL..89a1301A
Altcode: 2002nucl.ex...4008S; 2002nucl.ex...4008C
  Observations of neutral-current ν interactions on deuterium in
  the Sudbury Neutrino Observatory are reported. Using the neutral
  current (NC), elastic scattering, and charged current reactions
  and assuming the standard <SUP>8</SUP>B shape, the ν<SUB>e</SUB>
  component of the <SUP>8</SUP>B solar flux is φ<SUB>e</SUB> =
  1.76<SUP>+0.05</SUP><SUB>-0.05</SUB>(stat)<SUP>+0.09</SUP><SUB>-
  0.09</SUB>(syst)×10<SUP>6</SUP> cm<SUP>-2</SUP>
  s<SUP>-1</SUP> for a kinetic energy threshold of 5 MeV. The
  non- ν<SUB>e</SUB> component is φ<SUB>μτ</SUB> =
  3.41<SUP>+0.45</SUP><SUB>-0.45</SUB>(stat)<SUP>+0.48</SUP><SUB>-
  0.45</SUB>(syst)×10<SUP>6</SUP> cm<SUP>-2</SUP>
  s<SUP>-1</SUP>, 5.3σ greater than zero, providing strong
  evidence for solar ν<SUB>e</SUB> flavor transformation. The
  total flux measured with the NC reaction is φ<SUB>NC</SUB> =
  5.09<SUP>+0.44</SUP><SUB>-0.43</SUB>(stat)<SUP>+0.46</SUP><SUB>-
  0.43</SUB>(syst)×10<SUP>6</SUP> cm<SUP>-2</SUP> s<SUP>-1</SUP>,
  consistent with solar models.

Title: Measurement of Day and Night Neutrino Energy Spectra at SNO
    and Constraints on Neutrino Mixing Parameters
Authors: Ahmad, Q. R.; Allen, R. C.; Andersen, T. C.; Anglin, J. D.;
   Barton, J. C.; Beier, E. W.; Bercovitch, M.; Bigu, J.; Biller, S. D.;
   Black, R. A.; Blevis, I.; Boardman, R. J.; Boger, J.; Bonvin, E.;
   Boulay, M. G.; Bowler, M. G.; Bowles, T. J.; Brice, S. J.; Browne,
   M. C.; Bullard, T. V.; Bühler, G.; Cameron, J.; Chan, Y. D.; Chen,
   H. H.; Chen, M.; Chen, X.; Cleveland, B. T.; Clifford, E. T.; Cowan,
   J. H.; Cowen, D. F.; Cox, G. A.; Dai, X.; Dalnoki-Veress, F.; Davidson,
   W. F.; Doe, P. J.; Doucas, G.; Dragowsky, M. R.; Duba, C. A.; Duncan,
   F. A.; Dunford, M.; Dunmore, J. A.; Earle, E. D.; Elliott, S. R.;
   Evans, H. C.; Ewan, G. T.; Farine, J.; Fergani, H.; Ferraris, A. P.;
   Ford, R. J.; Formaggio, J. A.; Fowler, M. M.; Frame, K.; Frank, E. D.;
   Frati, W.; Gagnon, N.; Germani, J. V.; Gil, S.; Graham, K.; Grant,
   D. R.; Hahn, R. L.; Hallin, A. L.; Hallman, E. D.; Hamer, A. S.;
   Hamian, A. A.; Handler, W. B.; Haq, R. U.; Hargrove, C. K.; Harvey,
   P. J.; Hazama, R.; Heeger, K. M.; Heintzelman, W. J.; Heise, J.;
   Helmer, R. L.; Hepburn, J. D.; Heron, H.; Hewett, J.; Hime, A.; Howe,
   M.; Hykawy, J. G.; Isaac, M. C.; Jagam, P.; Jelley, N. A.; Jillings,
   C.; Jonkmans, G.; Kazkaz, K.; Keener, P. T.; Klein, J. R.; Knox, A. B.;
   Komar, R. J.; Kouzes, R.; Kutter, T.; Kyba, C. C.; Law, J.; Lawson,
   I. T.; Lay, M.; Lee, H. W.; Lesko, K. T.; Leslie, J. R.; Levine, I.;
   Locke, W.; Luoma, S.; Lyon, J.; Majerus, S.; Mak, H. B.; Maneira, J.;
   Manor, J.; Marino, A. D.; McCauley, N.; McDonald, A. B.; McDonald,
   D. S.; McFarlane, K.; McGregor, G.; Meijer Drees, R.; Mifflin,
   C.; Miller, G. G.; Milton, G.; Moffat, B. A.; Moorhead, M.; Nally,
   C. W.; Neubauer, M. S.; Newcomer, F. M.; Ng, H. S.; Noble, A. J.;
   Norman, E. B.; Novikov, V. M.; O'Neill, M.; Okada, C. E.; Ollerhead,
   R. W.; Omori, M.; Orrell, J. L.; Oser, S. M.; Poon, A. W.; Radcliffe,
   T. J.; Roberge, A.; Robertson, B. C.; Robertson, R. G.; Rosendahl,
   S. S.; Rowley, J. K.; Rusu, V. L.; Saettler, E.; Schaffer, K. K.;
   Schwendener, M. H.; Schülke, A.; Seifert, H.; Shatkay, M.; Simpson,
   J. J.; Sims, C. J.; Sinclair, D.; Skensved, P.; Smith, A. R.; Smith,
   M. W.; Spreitzer, T.; Starinsky, N.; Steiger, T. D.; Stokstad, R. G.;
   Stonehill, L. C.; Storey, R. S.; Sur, B.; Tafirout, R.; Tagg, N.;
   Tanner, N. W.; Taplin, R. K.; Thorman, M.; Thornewell, P. M.; Trent,
   P. T.; Tserkovnyak, Y. I.; van Berg, R.; van de Water, R. G.; Virtue,
   C. J.; Waltham, C. E.; Wang, J. -X.; Wark, D. L.; West, N.; Wilhelmy,
   J. B.; Wilkerson, J. F.; Wilson, J. R.; Wittich, P.; Wouters, J. M.;
   Yeh, M.
Bibcode: 2002PhRvL..89a1302A
Altcode: 2002nucl.ex...4009S; 2002nucl.ex...4009C
  The Sudbury Neutrino Observatory (SNO) has measured day and night
  solar neutrino energy spectra and rates. For charged current events,
  assuming an undistorted <SUP>8</SUP>B spectrum, the night minus day
  rate is 14.0%+/-6.3%<SUP>+1.5</SUP><SUB>-1.4</SUB>% of the average
  rate. If the total flux of active neutrinos is additionally constrained
  to have no asymmetry, the ν<SUB>e</SUB> asymmetry is found to be
  7.0%+/-4.9%<SUP>+1.3</SUP><SUB>-1.2</SUB>%. A global solar neutrino
  analysis in terms of matter-enhanced oscillations of two active flavors
  strongly favors the large mixing angle solution.

Title: Magnetic Field Strengths and Structures from Radio Observations
    of Solar Active Regions
Authors: Zhang, Chang-Xi; Gelfreikh, G. B.; Wang, Jing-Xiu
Bibcode: 2002ChJAA...2..266Z
Altcode:
  Radio observations of some active regions (ARs) obtained with the
  Nobeyama radioheliograph at λ=1.76 cm are used for estimating the
  magnetic field strength in the upper chromosphere, based on thermal
  bremsstrahlung. The results are compared with the magnetic field
  strength in the photosphere from observations with the Solar Magnetic
  Field Telescope (SMFT) at Huairou Solar Observing Station of Beijing
  Astronomical Observatory. The difference in the magnetic field strength
  between the two layers seems reasonable. The solar radio maps of active
  regions obtained with the Nobeyama radioheliograph, both in total
  intensity (I-map) and in circular polarizations (V-map), are compared
  with the optical magnetograms obtained with the SMFT. The comparison
  between the radio map in circular polarization and the longitudinal
  photospheric magnetogram of a plage region suggests that the radio
  map in circular polarization is a kind of magnetogram of the upper
  chromosphere. The comparison of the radio map in total intensity with
  the photospheric vector magnetogram of an AR shows that the radio map
  in total intensity gives indications of magnetic loops in the corona,
  thus we have a method of defining the coronal magnetic structure from
  the radio I-maps at λ=1.76 cm. Analysing the I-maps, we identified
  three components: (a) a compact bright source; (b) a narrow elongated
  structure connecting two main magnetic islands of opposite polarities
  (observed in both the optical and radio magnetograms); (c) a wide,
  diffuse, weak component that corresponds to a wide structure in the
  solar active region which shows in most cases an S or a reversed
  S contour, which is probably due to the differential rotation of
  the Sun. The last two components suggest coronal loops on different
  spatial scales above the neutral line of the longitudinal photospheric
  magnetic field.

Title: Regularity of the north-south asymmetry of solar activity
Authors: Li, K. J.; Wang, J. X.; Xiong, S. Y.; Liang, H. F.; Yun,
   H. S.; Gu, X. M.
Bibcode: 2002A&A...383..648L
Altcode:
  In the present work, the dominant hemisphere of solar activity in each
  of solar cycles 12 to 22 has been clarified by calculating the actual
  probability of the hemispheric distribution of several solar activity
  phenomena using long-term observational records. An attempt is made
  to demonstrate that a long characteristic time scale, about 12-cycle
  length, is inferred to occur in solar activity.

Title: Can Asymmetry of Solar Activity be Extended into Extended
    Cycle?
Authors: Li, Ke-Jun; Wang, Jing-Xiu; Liang, Hong-Fei; Gu, Xiao-Ma
Bibcode: 2002ChJAA...2...66L
Altcode:
  With the use of the Royal Greenwich Observatory data set of sunspot
  groups, an attempt is made to examine the north-south asymmetry of
  solar activity in the ``extended'' solar cycles. It is inferred that
  the asymmetry established for individual solar cycles does not extend
  to the "extended" cycles.

Title: The Chandra Deep Field-South: The 1 Million Second Exposure
Authors: Rosati, P.; Tozzi, P.; Giacconi, R.; Gilli, R.; Hasinger, G.;
   Kewley, L.; Mainieri, V.; Nonino, M.; Norman, C.; Szokoly, G.; Wang,
   J. X.; Zirm, A.; Bergeron, J.; Borgani, S.; Gilmozzi, R.; Grogin,
   N.; Koekemoer, A.; Schreier, E.; Zheng, W.
Bibcode: 2002ApJ...566..667R
Altcode:
  We present the main results from our 940 ks observation of the Chandra
  Deep Field-South using the source catalog described in an accompanying
  paper by Giacconi et al. We extend the measurement of source number
  counts to 5.5×10<SUP>-17</SUP> ergs cm<SUP>-2</SUP> s<SUP>-1</SUP> in
  the soft 0.5-2 keV band and 4.5×10<SUP>-16</SUP> ergs cm<SUP>-2</SUP>
  s<SUP>-1</SUP> in the hard 2-10 keV band. The hard-band logN-logS
  shows a significant flattening (slope ~=0.6) below ~10<SUP>-14</SUP>
  ergs cm<SUP>-2</SUP> s<SUP>-1</SUP>, leaving at most 10%-15% of the
  X-ray background to be resolved, the main uncertainty lying in the
  measurement of the total flux of the X-ray background (XRB). On the
  other hand, the analysis in the very hard 5-10 keV band reveals a
  relatively steep logN-logS (slope ~=1.3) down to 10<SUP>-15</SUP>
  ergs cm<SUP>-2</SUP> s<SUP>-1</SUP>. Together with the evidence of
  a progressive flattening of the average X-ray spectrum near the flux
  limit, this indicates that there is still a nonnegligible population
  of faint hard sources to be discovered at energies not well probed
  by Chandra, which possibly contributes to the 30 keV bump in the
  spectrum of the XRB. We use optical redshifts and identifications,
  obtained with the Very Large Telescope, for one-quarter of the sample to
  characterize the combined optical and X-ray properties of the Chandra
  Deep Field-South sample. Different source types are well separated
  in a parameter space that includes X-ray luminosity, hardness ratio,
  and R-K color. Type II objects, while redder on average than the
  field population, have colors that are consistent with being hosted
  by a range of galaxy types. Type II active galactic nuclei are mostly
  found at z&lt;~1, in contrast with predictions based on active galactic
  nucleus population synthesis models, thus suggesting a revision of their
  evolutionary parameters. Based on observations made at the European
  Southern Observatory (ESO), the Paranal Observatory Office, Antofagasta,
  Chile. The ESO Imaging Survey observations have been carried out using
  the ESO New Technology Telescope (NTT) at the La Silla Observatory,
  Avenida, El Santo 1538, La Serena, Chile (ESO LP 164.O-O561).

Title: What Can We Learn From Constructing CME Models
Authors: Lin, J.; Wang, J. X.
Bibcode: 2002stma.conf..137L
Altcode:
  No abstract at ADS

Title: Magnetic Flux Cancellation Associated with Coronal Mass
    Ejections
Authors: Wang, J. X.; Zhang, J.; Deng, Y. Y.
Bibcode: 2002stma.conf...93W
Altcode:
  No abstract at ADS

Title: New Results from the X-Ray and Optical Survey of the Chandra
Deep Field-South: The 300 Kilosecond Exposure. II.
Authors: Tozzi, P.; Rosati, P.; Nonino, M.; Bergeron, J.; Borgani,
   S.; Gilli, R.; Gilmozzi, R.; Hasinger, G.; Grogin, N.; Kewley, L.;
   Koekemoer, A.; Norman, C.; Schreier, E.; Szokoly, G.; Wang, J. X.;
   Zheng, W.; Zirm, A.; Giacconi, R.
Bibcode: 2001ApJ...562...42T
Altcode: 2001astro.ph..3014T
  We present results from 300 ks of X-ray observations of the Chandra
  Deep Field-South. The field of the four combined exposures is now
  0.1035 deg<SUP>2</SUP>, and we reach a flux limit of 10<SUP>-16</SUP>
  ergs s<SUP>-1</SUP> cm<SUP>-2</SUP> in the 0.5-2 keV soft band and
  10<SUP>-15</SUP> ergs s<SUP>-1</SUP> cm<SUP>-2</SUP> in the 2-10
  keV hard band, i.e., a factor of 2 fainter than the previous 120
  ks exposure. The total catalog is composed of 197 sources including
  22 sources detected only in the hard band, 51 only in the soft band,
  and 124 detected in both bands. We now have the optical spectra for 86
  optical counterparts. The logN-logS relationship of the whole sample
  confirms the flattening with respect to the ASCA hard counts and the
  ROSAT soft counts. The average logarithmic slopes of the number counts
  are α=0.66+/-0.06 and α=0.92+/-0.12 in the soft and hard bands,
  respectively. Double power-law fits to the differential counts show
  evidence of further flattening at the very faint end to slopes of
  0.5+/-0.1 and 0.6+/-0.2 in the soft and hard bands, respectively. We
  compute the total contribution to the X-ray background (XRB) in the
  2-10 keV band, which now amounts to (1.45+/-0.15)×10<SUP>-11</SUP> ergs
  cm<SUP>-2</SUP> s<SUP>-1</SUP> deg<SUP>-2</SUP> (after the inclusion of
  the ASCA sources to account for the bright end) to a lower flux limit of
  10<SUP>-15</SUP> ergs s<SUP>-1</SUP> cm<SUP>-2</SUP>. This corresponds
  to 60%-90% of the unresolved hard XRB, given the uncertainties
  on its actual value. We confirm previous findings on the average
  spectrum of the sources, which is well described by a power law
  with Γ=1.44+/-0.03, and the progressive hardening of the sources at
  lower fluxes. In particular, we find that the average spectral slope
  of the sources is flatter than the average for fluxes lower than
  9×10<SUP>-15</SUP> ergs s<SUP>-1</SUP> cm<SUP>-2</SUP> in the hard
  band. The hardening of the spectra is consistent with an increasing
  fraction of absorbed objects (N<SUB>H</SUB>&gt;10<SUP>22</SUP>
  cm<SUP>-2</SUP>) at low fluxes. From 86 redshifts available at present,
  we find that hard sources have on average lower redshifts (z&lt;=1)
  than soft sources. Their typical luminosities and optical spectra
  show that most of these sources are obscured active galactic nuclei
  (AGNs), as expected by AGN population synthesis models of the XRB. We
  are still in the process of finding hard sources that constitute the
  remaining fraction of the total XRB. Most of the sources detected
  only in the soft band appear to be optically normal galaxies with
  luminosities L<SUB>X</SUB>~=10<SUP>40</SUP>-10<SUP>42</SUP> ergs
  s<SUP>-1</SUP>. This population appears to be a mix of normal galaxies,
  possibly with enhanced star formation, and galaxies with low-level
  nuclear activity. Based on observations performed at the European
  Southern Observatory, Paranal, Chile.

Title: Ultraviolet Broad Absorption Features and the Spectral Energy
    Distribution of the Quasar PG 1351+64
Authors: Zheng, W.; Kriss, G. A.; Wang, J. X.; Brotherton, M.; Oegerle,
   W. R.; Blair, W. P.; Davidsen, A. F.; Green, R. F.; Hutchings, J. B.;
   Kaiser, M. E.
Bibcode: 2001ApJ...562..152Z
Altcode: 2001astro.ph..7536Z
  We present a moderate-resolution (~20 km s<SUP>-1</SUP>) spectrum of
  the mini-broad absorption line quasar (QSO) PG 1351+64 between 915
  and 1180 Å, obtained with the Far Ultraviolet Spectroscopic Explorer
  (FUSE). Additional low-resolution spectra at longer wavelengths were
  also obtained with the Hubble Space Telescope (HST) and ground-based
  telescopes. Broad absorption is present on the blue wings of C III
  λ977, Lyβ, O VI λλ1032, 1038, Lyα, N V λλ1238, 1242, Si IV
  λλ1393, 1402, and C IV λλ1548, 1550. The absorption profile can be
  fitted with five components at velocities of ~-780, -1049, -1629, -1833,
  and -3054 km s<SUP>-1</SUP> with respect to the emission-line redshift
  of z=0.088. All the absorption components cover a large fraction of the
  continuum source, as well as the broad-line region. The O VI emission
  feature is very weak, and the O VI/Lyα flux ratio is 0.08, one of the
  lowest among low-redshift active galaxies and QSOs. The UV continuum
  shows a significant change in slope near 1050 Å in the rest frame. The
  steeper continuum shortward of the Lyman limit extrapolates well to the
  observed weak X-ray flux level. The absorbers' properties are similar
  to those of high-redshift broad absorption line QSOs. The derived total
  column density of the UV absorbers is on the order of 10<SUP>21</SUP>
  cm<SUP>-2</SUP>, unlikely to produce significant opacity above 1
  keV in the X-ray. Unless there is a separate, high-ionization X-ray
  absorber, the QSO's weak X-ray flux may be intrinsic. The ionization
  level of the absorbing components is comparable to that anticipated
  in the broad-line region; therefore, the absorbers may be related
  to broad-line clouds along the line of sight. Based on observations
  made for the Guaranteed Time Team by the NASA-CNES-CSA FUSE mission,
  operated by the Johns Hopkins University under NASA contract NAS
  5-32985, and observations with the NASA/ESA Hubble Space Telescope,
  obtained at the Space Telescope Science Institute, which is operated
  by the Association of Universities of Research in Astronomy, Inc.,
  under NASA contract NAS 5-26555.

Title: The Chandra Deep Field South: the 1 Million Second
Authors: Rosati, P.; Tozzi, P.; Giacconi, R.; Gilli, R.; Hasinger, G.;
   Kewley, L.; Mainieri, V.; Nonino, M.; Norman, C.; Szokoly, G.; Wang,
   J. X.; Zirm, A.; Bergeron, J.; Borgani, S.; Gilmozzi, R.; Grogin,
   N.; Koekemoer, A.; Schreier, E.; Zheng, W.
Bibcode: 2001astro.ph.10452R
Altcode:
  We present the main results from our 940 ksec observation of the Chandra
  Deep Field South (CDFS), using the source catalog described in an
  accompanying paper (Giacconi et al. 2001). We extend the measurement
  of source number counts to 5.5e-17 erg/cm^2/s in the soft 0.5-2 keV
  band and 4.5e-16 erg/cm^2/s in the hard 2-10 keV band. The hard band
  LogN-LogS shows a significant flattening (slope~=0.6) below ~1e-14
  erg/cm^2/s, leaving at most 10-15% of the X-ray background (XRB)
  to be resolved, the main uncertainty lying in the measurement of the
  total flux of the XRB. On the other hand, the analysis in the very
  hard 5-10 keV band reveals a relatively steep LogN-LogS (slope ~=1.3)
  down to 1e-15 erg/cm^2/s. Together with the evidence of a progressive
  flattening of the average X-ray spectrum near the flux limit, this
  indicates that there is still a non negligible population of faint
  hard sources to be discovered at energies not well probed by Chandra,
  which possibly contribute to the 30 keV bump in the spectrum of the
  XRB. We use optical redshifts and identifications, obtained with the
  VLT, for one quarter of the sample to characterize the combined optical
  and X-ray properties of the CDFS sample. Different source types are well
  separated in a parameter space which includes X-ray luminosity, hardness
  ratio and R-K color. Type II objects, while redder on average than the
  field population, have colors which are consistent with being hosted
  by a range of galaxy types. Type II AGN are mostly found at z&lt;~1,
  in contrast with predictions based on AGN population synthesis models,
  thus suggesting a revision of their evolutionary parameters.

Title: Measurement of the Rate of ν<SUB>e</SUB> + d --&gt; p + p +
    e<SUP>-</SUP> Interactions Produced by <SUP>8</SUP>B Solar Neutrinos
    at the Sudbury Neutrino Observatory
Authors: Ahmad, Q. R.; Allen, R. C.; Andersen, T. C.; Anglin, J. D.;
   Bühler, G.; Barton, J. C.; Beier, E. W.; Bercovitch, M.; Bigu,
   J.; Biller, S.; Black, R. A.; Blevis, I.; Boardman, R. J.; Boger,
   J.; Bonvin, E.; Boulay, M. G.; Bowler, M. G.; Bowles, T. J.; Brice,
   S. J.; Browne, M. C.; Bullard, T. V.; Burritt, T. H.; Cameron, K.;
   Cameron, J.; Chan, Y. D.; Chen, M.; Chen, H. H.; Chen, X.; Chon,
   M. C.; Cleveland, B. T.; Clifford, E. T.; Cowan, J. H.; Cowen,
   D. F.; Cox, G. A.; Dai, Y.; Dai, X.; Dalnoki-Veress, F.; Davidson,
   W. F.; Doe, P. J.; Doucas, G.; Dragowsky, M. R.; Duba, C. A.; Duncan,
   F. A.; Dunmore, J.; Earle, E. D.; Elliott, S. R.; Evans, H. C.; Ewan,
   G. T.; Farine, J.; Fergani, H.; Ferraris, A. P.; Ford, R. J.; Fowler,
   M. M.; Frame, K.; Frank, E. D.; Frati, W.; Germani, J. V.; Gil, S.;
   Goldschmidt, A.; Grant, D. R.; Hahn, R. L.; Hallin, A. L.; Hallman,
   E. D.; Hamer, A.; Hamian, A. A.; Haq, R. U.; Hargrove, C. K.; Harvey,
   P. J.; Hazama, R.; Heaton, R.; Heeger, K. M.; Heintzelman, W. J.;
   Heise, J.; Helmer, R. L.; Hepburn, J. D.; Heron, H.; Hewett, J.;
   Hime, A.; Howe, M.; Hykawy, J. G.; Isaac, M. C.; Jagam, P.; Jelley,
   N. A.; Jillings, C.; Jonkmans, G.; Karn, J.; Keener, P. T.; Kirch,
   K.; Klein, J. R.; Knox, A. B.; Komar, R. J.; Kouzes, R.; Kutter, T.;
   Kyba, C. C.; Law, J.; Lawson, I. T.; Lay, M.; Lee, H. W.; Lesko, K. T.;
   Leslie, J. R.; Levine, I.; Locke, W.; Lowry, M. M.; Luoma, S.; Lyon,
   J.; Majerus, S.; Mak, H. B.; Marino, A. D.; McCauley, N.; McDonald,
   A. B.; McDonald, D. S.; McFarlane, K.; McGregor, G.; McLatchie, W.;
   Drees, R. Meijer; Mes, H.; Mifflin, C.; Miller, G. G.; Milton, G.;
   Moffat, B. A.; Moorhead, M.; Nally, C. W.; Neubauer, M. S.; Newcomer,
   F. M.; Ng, H. S.; Noble, A. J.; Norman, E. B.; Novikov, V. M.; O'Neill,
   M.; Okada, C. E.; Ollerhead, R. W.; Omori, M.; Orrell, J. L.; Oser,
   S. M.; Poon, A. W.; Radcliffe, T. J.; Roberge, A.; Robertson, B. C.;
   Robertson, R. G.; Rowley, J. K.; Rusu, V. L.; Saettler, E.; Schaffer,
   K. K.; Schuelke, A.; Schwendener, M. H.; Seifert, H.; Shatkay, M.;
   Simpson, J. J.; Sinclair, D.; Skensved, P.; Smith, A. R.; Smith, M. W.;
   Starinsky, N.; Steiger, T. D.; Stokstad, R. G.; Storey, R. S.; Sur,
   B.; Tafirout, R.; Tagg, N.; Tanner, N. W.; Taplin, R. K.; Thorman,
   M.; Thornewell, P.; Trent, P. T.; Tserkovnyak, Y. I.; van Berg, R.;
   van de Water, R. G.; Virtue, C. J.; Waltham, C. E.; Wang, J. -X.;
   Wark, D. L.; West, N.; Wilhelmy, J. B.; Wilkerson, J. F.; Wilson,
   J.; Wittich, P.; Wouters, J. M.; Yeh, M.
Bibcode: 2001PhRvL..87g1301A
Altcode: 2001nucl.ex...6015S; 2001nucl.ex...6015C
  Solar neutrinos from <SUP>8</SUP>B decay have been detected
  at the Sudbury Neutrino Observatory via the charged current
  (CC) reaction on deuterium and the elastic scattering (ES) of
  electrons. The flux of ν<SUB>e</SUB>'s is measured by the
  CC reaction rate to be φ<SUP>CC</SUP>(ν<SUB>e</SUB>)
  = 1.75+/-0.07(stat)<SUP>+0.12</SUP><SUB>-
  0.11</SUB>(syst)+/-0.05(theor)×10<SUP>6</SUP> cm<SUP>-2</SUP>
  s<SUP>-1</SUP>. Comparison of φ<SUP>CC</SUP>(ν<SUB>e</SUB>) to
  the Super-Kamiokande Collaboration's precision value of the flux
  inferred from the ES reaction yields a 3.3σ difference, assuming the
  systematic uncertainties are normally distributed, providing evidence
  of an active non- ν<SUB>e</SUB> component in the solar flux. The
  total flux of active <SUP>8</SUP>B neutrinos is determined to be
  5.44+/-0.99×10<SUP>6</SUP> cm<SUP>-2</SUP> s<SUP>-1</SUP>.

Title: Resolving the X-ray background with Chandra: the 1 MS
    observation of the Chandra Deep Field South *
Authors: Tozzi, P.; Bergeron, J.; Borgani, S.; Giacconi, R.; Gilli,
   R.; Gilmozzi, R.; Grogin, N.; Hasinger, G.; Kellerman, K.; Kewley,
   L.; Koekemoer, A.; Mainier, V.; Nonino, M.; Norman, C.; Rosati, P.;
   Schreier, E.; Shaver, P.; Szokoly, G.; Wang, J. X.; Zheng, W.; Zirm, A.
Bibcode: 2001cghr.confE..66T
Altcode:
  No abstract at ADS

Title: The Chandra Deep Field South
Authors: Giacconi, R.; Rosati, P.; Tozzi, P.; Borgani, S.; Hasinger,
   G.; Bergeron, J.; Gilmozzi, R.; Nonino, M.; Gilli, R.; Zirm, A.;
   Wang, J. X.; Zheng, W.; Kellermann, K. I.; Shaver, P.; Schreier, E.;
   Koekemoer, A.; Grogin, N.; Norman, C.
Bibcode: 2000AAS...197.9001G
Altcode: 2000BAAS...32.1562G
  We present results from the on-going ultra deep Chandra observations
  in the Chandra Deep Field South (CDF-S). As of October 2000, we
  have collected an exposure of 300 ksec which covers an area of 0.1
  deg<SUP>2</SUP>. These new data confirm and strengthen some of the
  conclusions of our initial analysis based on 130ksec observations
  (Giacconi et al. 2000). At the current depth, the source surface density
  is 3000/deg<SUP>2</SUP>. Number counts in the hard band (2-10keV)
  have overtaken the soft (0.5-2) counts and show evidence of flattening
  below 10<SUP>-15</SUP> erg/cm<SUP>2</SUP>/s [2-10 keV]. The hardening
  of the source spectra continues to fainter fluxes, most likely the
  result of an increasing absorption column. We discuss the implications
  of these observations in light of new population synthesis models. We
  will also show the spectro-photometric and morphological properties
  of the optical counterparts from the on-going source identification
  program with the VLT and HST/WFPC2. We acknowledge support from NASA
  grants NAG-8-1527 and NAG-8-1133.

Title: The X-Ray Absorber in Broad Absorption Line Quasars
Authors: Wang, T. G.; Brinkmann, W.; Yuan, W.; Wang, J. X.; Zhou, Y. Y.
Bibcode: 2000ApJ...545...77W
Altcode: 2000astro.ph..8291W
  Recent observations of Broad Absorption Line (BAL) quasars demonstrated
  that the soft X-ray emission of these objects is extremely weak, and
  convincing evidence for very strong absorption by a high column density
  (~10<SUP>23.5</SUP> cm<SUP>-2</SUP>) was obtained for PG 1411+442,
  even though it is one of the few BAL QSOs strongly detected in soft
  X-rays. This paper examines the ionization status and geometry of
  the X-ray absorber by combining the properties of the UV lines with
  the X-ray continuum absorption. We show that the gas has to have
  large column densities in ions of major UV absorption lines, such
  as C IV, N V, O VI, and Ne VIII, in order to have sufficient opacity
  around 0.2-0.35 keV. The UV absorption lines have to be saturated if
  the X-ray absorber intersects the line of sight to the UV continuum
  emission region. A uniformly covering UV and X-ray absorption model can
  be constructed for PG 1411+442, but in some other soft X-ray-detected
  BAL QSOs, such as PG 1001+054, the observed line optical depth is much
  lower than expected from the X-ray-absorbing material. We propose a
  scheme in which a substantial fraction of the line of sight to the
  continuum source may be covered by either an optically thick flow or
  clouds in a narrow velocity range, but in which the total covering
  factor of either the whole flow or all clouds is close to unity. The
  absorber can contribute significantly to the extremely highly ionized
  emission lines, such as O VI λλ1032/1037 and Ne VIII λλ770/780,
  if it covers a substantial fraction of solid angle and if the density
  is higher than 10<SUP>8</SUP> cm<SUP>-3</SUP>. However, it has very
  little impact on the medium- and low-ionization UV lines such as N V
  and C IV. The profiles of Ne VIII and O VI lines may be indicators for
  the kinematics of the X-ray absorber in QSOs. The observed Ne VIII line
  profiles in QSOs suggest that the velocity of the gas projected onto our
  line of sight is similar to that seen in the outflows of the UV BALs.

Title: The Sudbury Neutrino Observatory
Authors: Boger, J.; Hahn, R. L.; Rowley, J. K.; Carter, A. L.;
   Hollebone, B.; Kessler, D.; Blevis, I.; Dalnoki-Veress, F.; DeKok,
   A.; Farine, J.; Grant, D. R.; Hargrove, C. K.; Laberge, G.; Levine,
   I.; McFarlane, K.; Mes, H.; Noble, A. T.; Novikov, V. M.; O'Neill,
   M.; Shatkay, M.; Shewchuk, C.; Sinclair, D.; Clifford, E. T. H.; Deal,
   R.; Earle, E. D.; Gaudette, E.; Milton, G.; Sur, B.; Bigu, J.; Cowan,
   J. H. M.; Cluff, D. L.; Hallman, E. D.; Haq, R. U.; Hewett, J.; Hykawy,
   J. G.; Jonkmans, G.; Michaud, R.; Roberge, A.; Roberts, J.; Saettler,
   E.; Schwendener, M. H.; Seifert, H.; Sweezey, D.; Tafirout, R.;
   Virtue, C. J.; Beck, D. N.; Chan, Y. D.; Chen, X.; Dragowsky, M. R.;
   Dycus, F. W.; Gonzalez, J.; Isaac, M. C. P.; Kajiyama, Y.; Koehler,
   G. W.; Lesko, K. T.; Moebus, M. C.; Norman, E. B.; Okada, C. E.; Poon,
   A. W. P.; Purgalis, P.; Schuelke, A.; Smith, A. R.; Stokstad, R. G.;
   Turner, S.; Zlimen, I.; Anaya, J. M.; Bowles, T. J.; Brice, S. J.;
   Esch, E. -I.; Fowler, M. M.; Goldschmidt, A.; Hime, A.; McGirt,
   A. F.; Miller, G. G.; Teasdale, W. A.; Wilhelmy, J. B.; Wouters,
   J. M.; Anglin, J. D.; Bercovitch, M.; Davidson, W. F.; Storey, R. S.;
   Biller, S.; Black, R. A.; Boardman, R. J.; Bowler, M. G.; Cameron, J.;
   Cleveland, B.; Ferraris, A. P.; Doucas, G.; Heron, H.; Howard, C.;
   Jelley, N. A.; Knox, A. B.; Lay, M.; Locke, W.; Lyon, J.; Majerus,
   S.; Moorhead, M.; Omori, M.; Tanner, N. W.; Taplin, R. K.; Thorman,
   M.; Wark, D. L.; West, N.; Barton, J. C.; Trent, P. T.; Kouzes, R.;
   Lowry, M. M.; Bell, A. L.; Bonvin, E.; Boulay, M.; Dayon, M.; Duncan,
   F.; Erhardt, L. S.; Evans, H. C.; Ewan, G. T.; Ford, R.; Hallin, A.;
   Hamer, A.; Hart, P. M.; Harvey, P. J.; Haslip, D.; Hearns, C. A. W.;
   Heaton, R.; Hepburn, J. D.; Jillings, C. J.; Korpach, E. P.; Lee,
   H. W.; Leslie, J. R.; Liu, M. -Q.; Mak, H. B.; McDonald, A. B.;
   MacArthur, J. D.; McLatchie, W.; Moffat, B. A.; Noel, S.; Radcliffe,
   T. J.; Robertson, B. C.; Skensved, P.; Stevenson, R. L.; Zhu, X.; Gil,
   S.; Heise, J.; Helmer, R. L.; Komar, R. J.; Nally, C. W.; Ng, H. S.;
   Waltham, C. E.; Allen, R. C.; Bühler, G.; Chen, H. H.; Aardsma, G.;
   Andersen, T.; Cameron, K.; Chon, M. C.; Hanson, R. H.; Jagam, P.; Karn,
   J.; Law, J.; Ollerhead, R. W.; Simpson, J. J.; Tagg, N.; Wang, J. -X.;
   Alexander, C.; Beier, E. W.; Cook, J. C.; Cowen, D. F.; Frank, E. D.;
   Frati, W.; Keener, P. T.; Klein, J. R.; Mayers, G.; McDonald, D. S.;
   Neubauer, M. S.; Newcomer, F. M.; Pearce, R. J.; de Water, R. G. V.;
   Berg, R. V.; Wittich, P.; Ahmad, Q. R.; Beck, J. M.; Browne, M. C.;
   Burritt, T. H.; Doe, P. J.; Duba, C. A.; Elliott, S. R.; Franklin,
   J. E.; Germani, J. V.; Green, P.; Hamian, A. A.; Heeger, K. M.; Howe,
   M.; Drees, R. M.; Myers, A.; Robertson, R. G. H.; Smith, M. W. E.;
   Steiger, T. D.; Wechel, T. V.; Wilkerson, J. F.
Bibcode: 2000NIMPA.449..172B
Altcode: 1999nucl.ex..10016C; 1999nucl.ex..10016T
  The Sudbury Neutrino Observatory is a second-generation water Cherenkov
  detector designed to determine whether the currently observed
  solar neutrino deficit is a result of neutrino oscillations. The
  detector is unique in its use of D<SUB>2</SUB>O as a detection medium,
  permitting it to make a solar model-independent test of the neutrino
  oscillation hypothesis by comparison of the charged- and neutral-current
  interaction rates. In this paper the physical properties, construction,
  and preliminary operation of the Sudbury Neutrino Observatory are
  described. Data and predicted operating parameters are provided
  whenever possible.

Title: X-Ray and Ultraviolet Spectral Properties of the X-Ray
    Transient Quasar PG 0844+349
Authors: Wang, T. G.; Brinkmann, W.; Matsuoka, M.; Wang, J. X.;
   Yuan, W.
Bibcode: 2000ApJ...533..113W
Altcode:
  Despite the fact that quasars are generally strong X-ray emitters,
  ROSAT discovered several objects with only very weak X-ray emission. In
  this paper, the X-ray data from ASCA and ROSAT and the UV spectra
  from Hubble Space Telescope (HST) and IUE of one of these quasars,
  PG 0844+349, are analyzed. The ROSAT spectrum can be well fitted by a
  single power law with Galactic absorption. No spectral variations were
  observed during changes of the 0.1-2.4 keV X-ray flux by a factor of 10
  between the ROSAT All-Sky Survey and pointed observations, separated
  by 6 months. The ASCA satellite found the object in a high state with
  a photon index of 1.98 and an Fe Kα line with EW~300 eV. The X-ray
  flux in the 2-10 keV band is highly variable; the fastest variation
  detected is 60% in less than 2×10<SUP>4</SUP> s. The measured excess
  variance fits well the excess variance versus L<SUB>2-10keV</SUB>
  relation for Seyfert 1 galaxies; the flux variability in the 0.5-2.0 keV
  band shows a slightly higher amplitude than in the 2-10 keV band. We
  show that the optical microvariability of this object can actually be
  driven by reprocessing of the variable X-ray flux if one-half of the
  absorbed X-rays are reradiated in the optical-to-UV band. A weak broad
  intrinsic absorption line (FWHM~=800 km s<SUP>-1</SUP>), most likely
  Lyα absorption blueshifted by a velocity ~=-6000 km s<SUP>-1</SUP>
  relative to the quasar's rest frame, is found in the HST Faint Object
  Spectrograph spectrum. A similar C IV broad absorption line may also
  be present in the low-resolution IUE spectrum. Historic light curves
  in the X-ray, UV, and optical bands indicate that the variability
  amplitude in the UV and optical bands is much smaller than in the X-ray
  band. The QSO can be classified as X-ray weak only on one occasion
  out of five X-ray observations. An analysis of the long-term behavior
  of several other X-ray-weak objects shows no indications of a similar
  large X-ray variability.

Title: Ionized ultraviolet and soft X-ray absorption in the
    low-redshift active galactic nucleus PG 1126-041
Authors: Wang, T. G.; Brinkmann, W.; Wamsteker, W.; Yuan, W.; Wang,
   J. X.
Bibcode: 1999MNRAS.307..821W
Altcode: 1999astro.ph..3428W
  We present here the analysis of ultraviolet spectra from IUE and
  an X-ray spectrum from ROSAT PSPC observations of the X-ray-weak,
  far-infrared-loud AGN, PG 1126-041 (Mrk 1298). The first UV spectra
  taken in 1992 June, simultaneously with ROSAT, show strong absorption
  lines of Nv, Civ and Siiv, extending over a velocity range from -1000
  to -5000kms^-1 with respect to the corresponding line centre. Our
  analysis shows that the broad emission-line region (BELR) is, at least
  partially, covered by the material causing these absorption lines. In
  the IUE spectrum taken in 1995 January, the continuum was a factor of
  2 brighter and the UV absorption lines are found to be considerably
  weaker than in 1992, but little variation in the emission-line fluxes
  is found. With UV spectral indices of alpha_UV~=1.82 and 1.46 for
  the 1992 and 1995 data, the far-UV spectrum is steep. Based on the
  emission-line ratios and the broad-band spectral energy distribution, we
  argue that the steepness of the UV spectrum is unlikely to be caused by
  reddening. The soft X-ray emission in the ROSAT band is weak. A simple
  power-law model yields a very poor fit with a UV-to-X-ray spectral
  index alpha_UVX=2.3. Highly ionized (warm) absorption is suggested
  by the ROSAT data. After correcting for a warm absorber, the optical
  to X-ray spectral slope is close to the average of alpha_UVX~=1.67
  for radio-quiet quasars. From photoionization calculations we find
  the following results. (1) A single-zone absorption model cannot
  explain simultaneously the UV absorption lines and the ionized X-ray
  absorption if metal abundances are solar. Furthermore, in order to be
  consistent with the equivalent width of the observed Lyalpha absorption
  line, the turbulent velocity of the warm absorber must be less than
  190kms^-1, which imposes serious constraints on a disc wind model. (2)
  The UV absorption lines and their variability cannot be explained by
  a single-zone model with solar abundances and the large variability
  in the absorption lines suggests that Civ and Nv absorption lines are
  not severely saturated. (3) The absorption of the ionizing continuum
  by warm material strongly affects the emission-line spectrum.

Title: How Saturated Are Absorption Lines in the Broad Absorption
    Line Quasar PG 1411+442?
Authors: Wang, T. G.; Wang, J. X.; Brinkmann, W.; Matsuoka, M.
Bibcode: 1999ApJ...519L..35W
Altcode: 1999astro.ph..5054W
  Recently, convincing evidence was found for extremely large
  X-ray absorption by column densities greater than 10<SUP>23</SUP>
  cm<SUP>-2</SUP> in broad absorption line quasars. One consequence of
  this is that any soft X-ray emission from these QSOs would be the
  scattered light or leaked light from partially covering absorbing
  material. A detection of the unabsorbed soft X-ray and absorbed hard
  X-ray component will allow us to determine the total column density
  as well as the effective covering factor of the absorbing material,
  which are difficult to obtain from the UV absorption lines. Brinkmann
  et al. recently showed that both the unabsorbed and absorbed components
  are detected in the nearby very bright broad absorption line quasar PG
  1411+442. In this Letter, we make a further analysis of the broadband
  X-ray spectrum and the UV spectrum from the Hubble Space Telescope
  and demonstrate that broad absorption lines are completely saturated
  at the bottom of absorption troughs.

Title: Rapidly Variable Fe Kα Line in NGC 4051
Authors: Wang, J. X.; Zhou, Y. Y.; Xu, H. G.; Wang, T. G.
Bibcode: 1999ApJ...516L..65W
Altcode: 1999astro.ph..4321W
  We present a detailed analysis on the variability of the Fe K
  emission line in NGC 4051 using ASCA data. Through simple Gaussian
  line fits, we find not only obvious Fe K line variability with
  no significant difference in the X-ray continuum flux between
  two ASCA observations that were separated by ~ 440 days, but also
  rapid variability of the Fe K line on timescales ~10<SUP>4</SUP>
  s within the second observation. During the second observation, the
  line is strong (EW=733<SUP>+206</SUP><SUB>-219</SUB> eV) and broad
  (σ=0.96<SUP>+0.49</SUP><SUB>-0.35</SUB> keV) when the source is
  brightest and becomes weaker (EW=165<SUP>+87</SUP><SUB>-86</SUB> eV) and
  narrower (σ&lt;0.09 keV) while the source is weakest. The equivalent
  width of the Fe K line correlates positively with the continuum flux,
  which shows an opposite trend with another Seyfert type 1 galaxy,
  MCG -6-30-15.

Title: Solar sympathetic flares in two adjacent active regions
Authors: Shi, Zhong-Xian; Wang, Jing-Xiu; Luan, Di
Bibcode: 1997AcASn..38..257S
Altcode:
  We describe the magnetic configurations of a group of two-ribbon flares
  in NOAA 6233 and their temporally correlated one-ribbon flares in NOAA
  6240, and also the topological connectivity between the two active
  regions. The analyses show that the three one-ribbon flares took place
  in a unipolar flux region of positive polarity, which seems to be
  connected through a set of high-lying magnetic loops with the strong
  delta-sunspot, where the corresponding two-ribbon flares appeared. The
  interaction between the high-lying magnetic loops and the low-lying
  sheared magnetic loops in the delta-sunspot appears to be the primary
  cause for the two-ribbon flares. The accelerated electrons in the
  primary energy release may propagate along the high-lying magnetic loops
  (or the relevant separatrices), and result in the one-ribbon flares
  in NOAA 6240. Therefore, we suggest that these one-ribbon flares are
  the sympathetic flares of the correlated two-ribbon flares in NOAA 6233.

Title: Evolution of Magnetic Helicity in Magnetic Reconnection
Authors: Hu, Y. Q.; Xia, L. D.; Li, X.; Wang, J. X.; Ai, G. X.
Bibcode: 1997SoPh..170..283H
Altcode:
  This paper presents a definition of magnetic helicity specifically
  for two-dimensional magnetic fields and derives the associated
  helicity equation. The newly defined helicity is closely related to
  its three-dimensional counterpart and serves as a measure of the
  shear of magnetic field. Based on this, a numerical simulation is
  carried out on magnetic reconnection occurring in the lower solar
  atmosphere. It is found that the helicity dissipation due to magnetic
  reconnection is very small. A large amount of helicity is transferred
  upward and escapes from the domain of the solution, and the total
  helicity is approximately conserved during the magnetic reconnection
  and helicity transfer. This is in support of the applicability of
  a postulate, which was proposed by Taylor (1974, 1986) concerning
  the approximate conservation of magnetic helicity in the presence of
  resistive dissipation and magnetic reconnection in a highly conductive
  laboratory plasma, to the solar atmosphere.

Title: Book Review: Proceedings of the third China-Japan seminar on
    solar physics / International Academic Publishers, Beijing, 1995
Authors: Wang, J. X.; Ai, G. X.; Sakurai, T.; Hirayama, T.
Bibcode: 1996SoPh..169..225W
Altcode:
  No abstract at ADS

Title: Flares and velocity pattern around separatrix.
Authors: Shi, Zhong-xian; Wang, Jing-xiu
Bibcode: 1996ChA&A..20..305S
Altcode:
  A close relationship between flares and magnetic flux cancellation
  at the photospheric layer has been observationally established in a
  number of active regions. The flux cancellation precedes the flares
  by a few hours up to a day. During this time a specific pattern
  appears in the radial velocity field in the chromosphere, namely,
  the magnetic separatrix appears as a narrow blue-shifted band while
  the flares all occur in the red-shifted regions on either side. This
  observation supports the identification of flux cancellation with
  magnetic reconnection in the lower atmosphere and confirms that the
  reconnection is closely related to fast energy release in the corona.

Title: Magnetic Energy Buildup in a Quadrupole Field by Photospheric
    Shear Motion
Authors: Hu, Y. Q.; Wang, J. X.; Ai, G. X.; Nie, Y. P.
Bibcode: 1995SoPh..159..251H
Altcode:
  Using a two-dimensional, dissipative magnetohydrodynamic model,
  this paper presents a numerical simulation of the magnetic energy
  buildup in a quadrupolar field by photospheric shear motion. When
  electric current density is larger than a certain critical value,
  an anomalous resistivity is introduced in order to account for the
  dissipation caused by instabilities in high current regions. It is
  shown that like a bipolar field, a quadrupolar field can efficiently
  store magnetic free energy through photospheric shear motion. Electric
  current formed by shear concentrates on the separatrix and magnetic
  loops rooted in areas where the shear velocity gradient is large. The
  atmosphere is heated by anomalous resistive dissipation during the
  shear. Both magnetic and thermal energy increases nonlinearly with
  shearing displacement. When the anomalous resistivity increases or
  the critical current density decreases, the growth rate reduces for
  magnetic energy but goes up for thermal energy.

Title: On the transport of magnetic energy and complexity to the
    solar corona
Authors: Wang, Jing-xiu
Bibcode: 1995ChA&A..19..480W
Altcode:
  For the active corona—a system consisting of electromagnetic
  fields and particles, the only open field surface is the solar
  photosphere. Interaction between the velocity and magnetic fields on the
  photosphere is the primary cause of the upward transport of magnetic
  energy and complexity to the corona, with the diffusion process there
  also playing a role.

Title: Flares and separatrices between magnetic loops
Authors: Shi, Zhong-xian; Wang, Jing-xiu; Wang, Hai-min
Bibcode: 1995ChA&A..19..469S
Altcode:
  Time sequences of vector magnetograms of Hauirou and Big Bear
  Solar Observatories have provided us the opportunity to identify the
  individual magnetic loops and athe separatrices between them. Based on
  the continuous observatin of vector magnetic field of NOAA 7469 from
  4 to 12 April 1993, for the first time, the authors have identified
  the magnetic loop systems and relevant separatrices for such an active
  region. The observational signature ofthe cross-section of separatrices
  on the photosphere is as follows: (1) High degree of magnetic shear at
  or close to the separatrices; <P />(2) Steep gradient of line-of-sight
  magnetic field (∼ 0.1 G/km) crossing the neutral line. <P />(3)
  Flux cancellation from both sides of the separatrices. At this point
  the transverse field partly changes its alignment. <P />During the
  observed period, flare activity took place repeatedly in the vicinity
  of the separatrices.

Title: Preflare State
Authors: Rust, David M.; Sakurai, Takashi; Gaizauskas, Victor; Hofmann,
   Axel; Martin, Sara F.; Priest, Eric R.; Wang, Jing-Xiu
Bibcode: 1994SoPh..153....1R
Altcode:
  Discussion on the preflare state held at the Ottawa Flares 22
  Workshop focused on the interpretation of solar magnetograms and
  of Hα filament activity. Magnetograms from several observatories
  provided evidence of significant build up of electric currents in
  flaring regions. Images of X-ray emitting structures provided a clear
  example of magnetic relaxation in the course of a flare. Emerging
  and cancelling magnetic fields appear to be important for triggering
  flares and for the formation of filaments, which are associated with
  eruptive flares. Filaments may become unstable by the build up of
  electric current helicity. Examples of heliform eruptive filaments
  were presented at the Workshop. Theoretical models linking filaments
  and flares are briefly reviewed.

Title: A method for resolving the 180-degree ambiguity in the observed
    transverse field direction
Authors: Wang, Jing-Xiu
Bibcode: 1994ChA&A..18Q.355W
Altcode:
  No abstract at ADS

Title: A preliminary treatment of data from the full-disk magnetograph
Authors: Liu, Yang; Song, Guo-feng; Wang, Jing-shan; Wang, Jing-xiu
Bibcode: 1994ChA&A..18..319L
Altcode:
  A full-disk magnetogram obtained with the full-disk magnetograph of
  Huairou Solar Observing Station shows similar morphological features and
  magnetic field intensities as in traditional small scale magnetograms
  obtained by the solar magnetic field telescope at the same site.

Title: An Alternative Method for Removing the 180DEG Ambiguity of
    the Observed Transverse Field Direction
Authors: Wang, J. X.
Bibcode: 1994AcApS..14..166W
Altcode:
  No abstract at ADS

Title: A Study of Data Obtained by Full Disk Magnetograph
Authors: Liu, Y.; Song, G. F.; Wang, J. S.; Wang, J. X.
Bibcode: 1994AcApS..14..191L
Altcode:
  No abstract at ADS

Title: Shear Angle of Vector Magnetic Field
Authors: Lu, Y. P.; Wang, J. X.; Wang, H. N.
Bibcode: 1993AcApS..13..291L
Altcode:
  No abstract at ADS

Title: A New Method of Calculating the Vertical Current in Solar
    Active Regions
Authors: Wang, J. X.
Bibcode: 1993AcASn..34..436W
Altcode: 1993AcASn..34..438W
  No abstract at ADS

Title: An instance of the localized chromospheric polarity reversal
Authors: Wang, Jing-Xiu; Shi, Zhong-Xian
Bibcode: 1992ChA&A..16..325W
Altcode:
  At the chromospheric level, a localized magnetic feature with polarity
  opposite to the underlying photospheric magnetic field has been
  observed in a rapidly formed sunspot. The strength of this reversed
  polarity is several hundred gauss. Seven subflares, centering around
  the reversed polarity, have been identified in observation of nine
  hours. The flares showed progressive increase in size and extent with
  the develop- ment of the reversed polarity. The bipolar feature above
  the unipolar magnetic flux can only mean that a bundle of magnetic lines
  of force has been kinked or knotted, or a self-closed flux system has
  been developed above the photosphere.

Title: Lorentzian contributions to x-ray lineshapes in Si(Li)
    spectroscopy
Authors: Campbell, J. L.; Wang, J. -X.
Bibcode: 1992XRS....21..223C
Altcode:
  No abstract at ADS

Title: The relation between the twisting motion of a quiescent
    filament and the magnetic field
Authors: Shi, Zhong-Xian; Wang, Jing-Xiu
Bibcode: 1992ChA&A..16..350S
Altcode:
  The twisting motion of a quiescent filament in AR5572 was observed on 8
  July 1989. Based on the time sequence of magnetograms, Hβ fitergrams
  and Hβ Dopplergrams obtained at Huairou Solar Observing Station of
  Beijing Astronomical Observatory, the twisting motion of the filament
  is identified to be related to three cancelling magnetic features in
  the filament channel.

Title: Osmium-Iridium Correlation and Osmium Isotopic Composition
    in Some Geological Boundaries and Meteorites
Authors: Liu, Y. Z.; Wang, J. X.; Mao, X. Y.; Chai, C. F.
Bibcode: 1992Metic..27Q.251L
Altcode:
  Since the pioneering study of Alvarez et al. on K/T boundary event, Ir
  has long been considered to be the main indicator of extraterrestrial
  materials in boundaries, while little work about Os and its isotopic
  composition have been done. In this work a sophisticated radiochemical
  separation procedure together with neutron activation analsis (NAA)
  method was established for the determination of Os in some geological
  boundaries (P epsilon/epsilon, K/T, D/C, O/S, P/T). Combined with our
  early work--determination of Ir abundances [1], the sources of boundary
  events were deciphered by using the Os/Ir ratios. Simultaneously
  ^184Os/^190Os ratios in K/T boundaries, as well as inclusions of
  Allende chondrite and acid-insoluble residues of iron meteorites
  (Nandan, Jianshi, Longchang) were determined to search for the Os
  isotopic composition anomalies resulted from the extrasolar components
  by RNAA. The results show that the Os abundances exhibit a positive
  correlation with the Ir abundances for overall K/T boundary samples,
  but only the Os/Ir ratios of K/T boundaries, with the average of 0.98
  +- 0.55, are in excellent agreement with 1.01 of the solar system
  [2], Accordingly, it provides new evidence for an extraterrestrial
  source of the K/T event. The results of ^184Os/^190Os ratios,
  with uncertainties of less than 1%, indicate there is no remarkable
  ^184Os/^190Os ratio anomaly in the K/T boundary samples, which implies
  the impacting matter may be from the solar system not the extrasolar,
  while no anomaly exists in the inclusions of Allende chondrite and
  acid-insoluble residues of iron meteorites, which disagree with the
  results obtained by Goel [3]. REFERENCES [1] Chai Chifang (1988)
  Isotopenpraxis 24, pp. 257-272. [2] Anders E. and Grevesse N. (l989)
  Geochim. Cosmochim. Acta 53, 197-214. [3] Goel P.S.(1987) Proc. Indian
  Acad. Sci. (Earth Planet. Sci), 96, pp. 81-102.

Title: An approach to the development of magnetic shear
Authors: Wang, Jing-xiu
Bibcode: 1992ChA&A..16..207W
Altcode:
  In view of an approximate description of magnetic shear by non-potential
  character of a force-free magnetic field, the force-free factor
  α would be a measure of magnetic shear, and the shear development
  would be analytically described by a differential equation dα/dt=
  1/β <SUP>2</SUP>∇· G+ V·∇α, where, G = ∂B/∂t × B, might
  be called as the generation function of magnetic shear. It is clearly
  shown by this equation that the magnetic shear is generated by local
  dynamo action resulting from the interaction between magnetic field and
  plasma motion. It is also illustrated that the squeezing and pressing
  of opposite polarity fields, the flux emergence and submergence would
  be as effective as shear motion in producing magnetic shear.

Title: Direct indication of magnetic reconnection in solar photosphere
Authors: Wang, Jing-Xiu; Shi, Zhong-Xian
Bibcode: 1992AcApS..11..389W
Altcode:
  A direct indication of magnetic reconnection in solar photosphere
  has been found for the first time with the aid of the time sequence
  of vector magnetograms. The reconnection takes place in the interface
  between one pole of an emerging flux region and the old flux of opposite
  polarity. It occurs well after a subflare with X-ray classification
  of C2.9 when flux cancellation in the interface had lasted for several
  hours. It is suggested that the reconnection in the photosphere would
  be a common phenomenon on the sun.

Title: An example of localized chromospheric polarity reversal
Authors: Wang, Jing-Xiu; Shi, Zhong-Xian
Bibcode: 1992AcASn..33...95W
Altcode:
  In the chromosphere, a localized magnetic feature with polarity opposite
  to the underlying photospheric magnetic field is observed above a fast
  formed sunspot. The strength of this reversal polarity is as strong
  as several hundred gauss. Centering around the reversal polarity,
  seven subflares are observed during nine hours before and after the
  reversal. Each flare shows progressively increasing size and spatial
  extent with the development of the reversal polarity. The reversal
  polarity above the photosphere can only mean that the magnetic lines
  of force have been kinked, twisted or knotted, or a close flux system
  has been formed above the photosphere. This newly observed phenomenon
  has not yet been possible to predict by either the current sunspot
  models or flare models.

Title: Direct indication of magnetic reconnection in solar photosphere
Authors: Wang, Jing-xiu; Shi, Zhong-xian
Bibcode: 1992ChA&A..16...71W
Altcode:
  A direct indication of magnetic reconnection in solar photosphere
  has been found for the first time with the aid of the time sequence
  of vector magnetograms. The reconnection takes place in the interface
  between one pole of an emerging flux region and the old flux of opposite
  polarity. It occurs well after a subflare with X-ray classification
  of C2.9 when flux cancellation in the interface had lasted for several
  hours. It is suggested that the reconnection in the photosphere would
  be a common phenomenon on the sun.

Title: The Relation Between the Twisting Motion of a Quiescent
    Filament and the Magnetic Field
Authors: Shi, Z. X.; Wang, J. X.
Bibcode: 1992AcApS..12..196S
Altcode:
  No abstract at ADS

Title: Search for Celestial Gamma-Ray Point Sources with the Tibet
    Air Shower Array
Authors: Amenomori, M.; Bai, Z. W.; Cao, Z.; Ding, L. K.; Hibino, K.;
   Hotta, N.; Huang, Q.; Huo, A. X.; Jia, H. G.; Jiang, G. Z.; Jiao,
   S. Q.; Kajino, F.; Kasahara, K.; Labaciren; Mei, D. M.; Meng, L.;
   Mimaciren; Mizutani, K.; Mu, J.; Nanjo, H.; Nishizawa, M.; Nusang;
   Ohnishi, M.; Ohta, I.; Ren, J. R.; Saito, T.; Sakata, M.; Shi, Z. Z.;
   Shibata, M.; Shirai, T.; Sun, X. X.; Sugimoto, H.; Tai, A.; Taira,
   K.; Tan, Y. H.; Tateyama, N.; Torii, S.; Wang, H.; Wang, J. X.; Wen,
   C. Z.; Yamamoto, Y.; Yang, H. M.; Yu, G. C.; Yuan, P.; Yuda, T.; Zeng,
   J. G.; Zhao, C. H.; Zhang, C. S.; Zhang, H. M.; Zhang, L.; Zhasang;
   Zhou, W. D.
Bibcode: 1991ICRC....1..444A
Altcode: 1991ICRC...22a.444A
  No abstract at ADS

Title: Improved model for the intensity of low-energy tailing in
    Si(Li) x-ray spectra
Authors: Campbell, J. L.; Wang, J. -X.
Bibcode: 1991XRS....20..191C
Altcode:
  No abstract at ADS

Title: Two-dimensional power spectrum of small-scale magnetic fields
    on the quiet Sun
Authors: Wang, Jing-xiu; Shi, Zhong-xian; Liu, Jian-qiang
Bibcode: 1991ChA&A..15..239W
Altcode:
  No abstract at ADS

Title: Status and performance of the AS array of the Tibet
    AS<SUB>γ</SUB> experiment.
Authors: Tibet As Gamma Collaboration; Amenomori, M.; Bai, Z. W.; Cao,
   Z.; Ding, L. K.; Feng, Z. Y.; Hibino, K.; Hotta, N.; Huang, Q.; Huo,
   A. X.; Jia, H. Y.; Jiang, G. Z.; Jiao, S. Q.; Kajino, F.; Kasahara,
   K.; Labaciren; Mei, D. M.; Meng, L.; Mimaciren; Mizutani, K.; Mu, J.;
   Nanjo, H.; Nishizawa, M.; Nusang; Ohnishi, M.; Ohta, I.; Ren, J. R.;
   Saito, T.; Sakata, M.; Shi, Z. Z.; Shibata, M.; Shirai, T.; Sun, X. X.;
   Sugimoto, H.; Tai, A.; Taira, K.; Tan, Y. H.; Tateyama, N.; Torii,
   S.; Wang, H.; Wang, J. X.; Wen, C. Z.; Yamamoto, Y.; Yang, H. M.; Yu,
   G. C.; Yuan, P.; Yuda, T.; Zeng, J. G.; Zhao, C. H.; Zhang, C. S.;
   Zhang, H. M.; Zhang, L.; Zhang, M.; Zhasang; Zhaxiciren; Zhou, W. D.
Bibcode: 1991AIPC..220..257T
Altcode:
  The Tibet ASγ experiment, which has started since January, 1990, is
  located at an altitude of 4300 m at Yangbaging in Tibet, China (90.5°E,
  30.1°N). The air-shower array is composed of 49 scintillation counters
  for fast timing, each counter having an area of 0.5 m<SUP>2</SUP>, in
  a grid pattern with a spacing of 15 m and 16 density detectors. The
  analysis of experimental data shows that the performance of array
  is realized as expected by the Monte Carlo simulation. The detection
  threshold energy for γ-rays is ≡40 TeV; the peak energy 20 TeV. The
  angular resolution around 100 TeV is ≡0.5°. The systematic error of
  arrival direction is considerably smaller than the angular resolution
  in the concerned energy region.

Title: Performance of the AS array in Tibet for search for gamma-ray
    point sources.
Authors: Amenomori, M.; Bai, Z. W.; Cao, Z.; Ding, L. K.; Feng, Z. Y.;
   Hibino, K.; Hotta, N.; Huang, Q.; Huo, A. X.; Jia, H. Y.; Jiang,
   G. Z.; Jiao, S. Q.; Kajino, F.; Kasahara, K.; Labaciren; Mei, D. M.;
   Meng, L.; Mimaciren; Mizutani, K.; Mu, J.; Nanjo, H.; Nishizawa,
   M.; Nusang; Ohnishi, M.; Ohta, I.; Ren, J. R.; Saito, T.; Sakata,
   M.; Shi, Z. Z.; Shibata, M.; Shirai, T.; Sun, X. X.; Sugimoto, H.;
   Tai, A.; Taira, K.; Tan, Y. H.; Tateyama, N.; Torii, S.; Wang, H.;
   Wang, J. X.; Wen, C. Z.; Yamamoto, Y.; Yang, H. M.; Yu, G. C.; Yuan,
   P.; Yuda, T.; Zeng, J. G.; Zhao, C. H.; Zhang, C. S.; Zhang, H. M.;
   Zhang, L.; Zhang, M.; Zhasang; Zhaxiciren; Zhou, W. D.
Bibcode: 1991aame.confQ.449A
Altcode:
  No abstract at ADS

Title: Direct Evidence of Magnetic Reconnection in Photospheric
    Layer on the Sun
Authors: Wang, J. X.; Shi, Z. X.
Bibcode: 1991AcApS..11..389W
Altcode:
  No abstract at ADS

Title: Search for gamma-ray point sources by the fast-timing detector
    array in Tibet.
Authors: Amenomori, M.; Bai, Z. W.; Cao, Z.; Ding, L. K.; Feng, Z. Y.;
   Hibino, K.; Hotta, N.; Huang, Q.; Huo, A. X.; Jia, H. Y.; Jiang,
   G. Z.; Jiao, S. Q.; Kajino, F.; Kasahara, K.; Labaciren; Mei, D. M.;
   Meng, L.; Mimaciren; Mizutani, K.; Mu, J.; Nanjo, H.; Nishizawa,
   M.; Nusang; Ohnishi, M.; Ohta, I.; Ren, J. R.; Saito, T.; Sakata,
   M.; Shi, Z. Z.; Shibata, M.; Shirai, T.; Sun, X. X.; Sugimoto, H.;
   Tai, A.; Taira, K.; Tan, Y. H.; Tateyama, N.; Torii, S.; Wang, H.;
   Wang, J. X.; Wen, C. Z.; Yamamoto, Y.; Yang, H. M.; Yu, G. C.; Yuan,
   P.; Yuda, T.; Zeng, J. G.; Zhao, C. H.; Zhang, C. S.; Zhang, H. M.;
   Zhang, L.; Zhang, M.; Zhasang; Zhaxiciren; Zhou, W. D.
Bibcode: 1991aame.confR.449A
Altcode:
  As the first result of the Tibet experiment the data obtained during
  the week centered at the radio-burst from Cygnus X-3 on 15th of August,
  1990, were analysed. But the preliminary results do not give any excess
  from Cygnus X-3 in this period at the median energy 30 TeV.

Title: Fast appearances and disappearances of weak intranetwork
    magnetic fields
Authors: Shi, Zhong-xian; Wang, Jing-xiu; Liu, Jian-qiang; Han, Feng;
   Liu, Gui-lin
Bibcode: 1990ChA&A..14..325S
Altcode:
  Under good seeing conditions (&lt;2'), the high resolution magnetic
  field observation at Huairou Solar Observing Station'is capable of
  detecting the intranetwork field. An analysis of some magnetograms
  of 1988 September 5 shows: 1. That the observed weak intranetwork
  magnetic fields (WINF) with maximum flux B between 5 and 10 G are real
  structures. 2. That About 70% of the WINF became undetectable at ±
  5 G level after 3.4 min and about 30% can be seen again. 3. That the
  number of WINF seen decreased exponentially with time, from which
  we estimated an upper limit of about 3 min for the mean life of a
  WINF. 4. That a WINF is a collection of unresolved flux elements,
  with a flux between 2.0(+16) and 1.0(+18) mx. Our results are similar
  to those in the magnetograms of 1984 September 9 obtained by the Big
  Bear Solar Observatory.

Title: Two-dimensional power spectrum of small-scale magnetic fields
    on the quiet sun.
Authors: Wang, Jing-Xiu; Shi, Zhong-Xian; Liu, Jian-Qiang
Bibcode: 1990ChA&A..14..240W
Altcode: 1990ChA&A..14..240.
  No abstract at ADS

Title: Fast appearances and disappearances of weak intranetwork
    magnetic fields
Authors: Shi, Zhong-Xian; Wang, Jing-Xiu; Liu, Jian-Qiang; Han, Feng;
   Liu, Gui-Lin
Bibcode: 1990AcASn..31...63S
Altcode:
  Results are presented of the analysis of magnetograms obtained, under
  conditions of best visibility, at the Huairou Station of the Beijing
  Observatory on September 5, 1988. The magnetograms showed the existence
  of weak intranetwork magnetic fields (INFs) which were appearing
  and disappearing, with a maximum flux B between 5 and 10 G. Evidence
  is presented that the weak appearing and disappearing INFs are real
  structures; about 70 percent of INFs become undetectable at the level of
  about 5 G after 3.4 min of observation; about 30 percent of INFs can be
  seen again. The number of weak INFs decreases exponentially with time,
  leading to an upper limit of about 3 min for the mean life of a weak
  INF. It is suggested that a weak INF is a collection of unresolved
  flux elements, with a flux between 2.0(+16) and 1.0(+18) Mx.

Title: Two-dimensional power spectrum of small-scale magnetic fields
    on the quiet sun.
Authors: Wang, Jing-Xiu; Shi, Zhong-Xian; Liu, Jian-Qiang
Bibcode: 1990AcApS..10...96W
Altcode:
  Based on magnetograms of September 5, 1988, the authors constructed
  a 2-D power spectrum for small-scale magnetic fields in a solar quiet
  region. The preliminary results are summarized as follows. (1) The solar
  magnetic fields in quiet regions are not only concentrated in discrete
  flux patches, but also distributed over discrete spatial periods. (2)
  The most obvious periods of small-scale fields are of supergranule
  scales. There are some peaks in the power spectrum corresponding to
  the spatial periods in mesogranule scales, and to the scales in between
  meso- and supergranules.

Title: The observed size, flux spectrum of small-scale magnetic
    features.
Authors: Wang, Jing-Xiu; Shi, Zhong-Xian; Liu, Jian-Qiang; Feng, Han;
   Liu, Gui-Lin
Bibcode: 1989PBeiO..14...44W
Altcode:
  The observed size, flux spectrum, and spatial distribution of
  small-scale magnetic features on the quiet photosphere are obtained
  statistically based on the high sensitivity magnetograms acquired at
  Huairou Solar Observing Station of Beijing Astronomical Observatory. The
  implications of these observational results are briefly discussed.

Title: The relationship between solar flare and magnetic field in
    AR 5229.
Authors: Shi, Zhong-Xian; Wang, Jing-Xiu; Liu, Gui-Lin; Hang, Feng
Bibcode: 1989PYunO...1S..87S
Altcode:
  Active region 5229 was studied during 13 - 18 November 1988 using
  Hβ filtergrams and Fe I 5324 videomagnetograms acquired at Huairou
  Solar Observing Station of Beijing Astronomical Observatory. Newly
  emerging flux, magnetic shear and magnetic flux cancellation were
  examined according to the evolution of magnetic fields. Preliminary
  results of the analysis were summarized.

Title: An example of general solar-terrestrial effects of major
    solar events.
Authors: Gao, Mei-Qing; Liu, Chun-Jie; Wang, Jing-Xiu
Bibcode: 1989PYunO...1S.180G
Altcode:
  The general solar-terrestrial effects including 20 parameters of major
  solar events in February, 1986 are analyzed and illustrated in terms
  of time sequence of various disturbances in interplanetary space,
  ionosphere and geomagnetic field. The characteristics of geomagnetic
  storm recorded at 6 stations are compared. The satellite anomaly and
  communication disturbance are also shown.

Title: The Relationship Between Solar Flare and Magnetic Field
    in AR5229
Authors: Shi, Z. X.; Wang, J. X.; Liu, G. L.; Hang, F.
Bibcode: 1989PYunO..87....1S
Altcode:
  No abstract at ADS

Title: Interpolated Dirac-Fock Values of L-Subshell X-Ray Emission
    Rates Including Overlap and Exchange Effects
Authors: Campbell, J. L.; Wang, J. -X.
Bibcode: 1989ADNDT..43..281C
Altcode:
  Published theoretical L x-ray emission rates based upon a fixed atomic
  potential cover the atomic number range Z = 4 to 94. However, the
  presumably more accurate calculations employing different initial- and
  final-state potentials have been done for only 21 values of Z. The ratio
  of these two rates for each electric dipole transition as a function of
  Z is fitted using polynomials in piece-wise fashion. The fixed-potential
  emission rates are then renormalized by these interpolated ratios
  to provide equivalent two-potential rates. The errors incurred are
  generally under 0.2%.

Title: A Example of General Solar-Terrestrial Effects of Major
    Solar Events
Authors: Gao, M. Q.; Liu, C. J.; Wang, J. X.
Bibcode: 1989PYunO.180....1G
Altcode:
  No abstract at ADS

Title: The fine structure and evolution of a subflare.
Authors: Shi, Z. -X.; Chen, J.; Wang, J. -X.
Bibcode: 1988ChJSS...8....1S
Altcode:
  No abstract at ADS

Title: Samples from Martian Craters: Origin of the Martian Soil
    by Hydrothermal Alteration of Impact Melt Deposits and Atmospheric
    Interactions with Ejecta During Crater Formation
Authors: Wang, Jing-Xiu; Shi, Zhong-Xian
Bibcode: 1988AcASn..29...48W
Altcode:
  On July 9, 1984, continuous magnetograms with 1-2 arcsec spatial
  resolution, 2.5 min time resolution, and noise level below 5 Gauss
  were obtained. Analysis of these magnetograms after calibration and
  empirical corrections shows that, in addition to the transient,
  mixed polarity field described by Livingston and Harvey (1975),
  there is a stable type of unipolar flux form. These features have a
  typical size of 2-5 arcsecs in one dimension, a total flux of (+18)
  Mx, a field strength of approximately 40 G and a lifetime of several
  hours. The features are called intranetwork flux concentrations (INFC).

Title: Intra-network flux concentrations
Authors: Wang, Jing-xiu; Shi, Zhong-xian
Bibcode: 1988ChA&A..12..241W
Altcode:
  On 1984 July 9, we obtained continuous magnetograms with 1"-2" spatial
  resolution, 2.5min time resolution and noise level below 5 Gauss at
  Big Bear Solar Observatory. Analysis of' these magnetograms after
  calibration and empirical corrections shows that, in addition to the
  transient, mixed polarity field described by Livingston and Harvey
  (1975), there is a stable type of uni-polar flux forms. These features
  have a typical size of 2"-5" in one dimension, a total flux of (+18)
  Mx, a field strength of approximately 40G and a lifetime of several
  hours. We call these Intra-Network Flux Concentrations (INFC).

Title: The Structure and Evolution of Smallscale Magnetic Fields on
    the Solar Surface
Authors: Wang, J. X.; Shi, Z. X.
Bibcode: 1988PrA.....6..105W
Altcode:
  No abstract at ADS

Title: The structure and evolution of small-scale magnetic fields
    on the solar surface.
Authors: Wang, J. -X.; Shi, Z. -X.
Bibcode: 1988PABei...6...94W
Altcode:
  Small-scale magnetic fields on the solar surface, a term applied to all
  magnetic features and structures outside active regions, are usually
  much smaller in area than a supergranule. Currently they are divided
  into three categories: network magnetic fields, intranetwork magnetic
  fields and ephemeral active regions (or ephemeral regions). They are
  the majority of solar magnetic flux at any phase of solar cycle. Their
  appearance, disappearance and evolution may play an important role
  in heating the upper atmosphere. The observations of flux emergence,
  cancellation, coalescence and fragmentation cause us to view the
  network magnetic fields in a new way that the network fields are not
  only the products of the remnant fields of decaying active regions,
  but also the products of the remnant flux of ephemeral regions and
  intranetwork fields.

Title: Evolution of network magnetic fields of solar quiet regions
Authors: Shi, Zhong-xian; Wang, Jing-xiu
Bibcode: 1987ChA&A..11..221S
Altcode:
  There are 4 types of evolution patterns of network magnetic fields:
  (1) flux cancellation, the mutual disappearance of encountering fluxes
  of opposite polarity, (2) flux increase by emergence of ephemeral
  regions, (3) flux decrease of one polarity and (4) flux increase of one
  polarity, without emergence of ephemeral regions. From a time sequence
  of magnetograms of a quiet region of 1983 October 14, the evolution
  of 300 network features was measured. The magnetograms have a spatial
  resolution of 2 to 3 arcsec and a time resolution of about 2 hr. The
  statistics show that the contribution to flux decrease by Type 3 is
  1.28 times that by Type 1, and the contribution to flux increase by
  Type 4 is 7 times that by Type 2.

Title: Evolution of network magnetic fields of solar quiet regions
Authors: Shi, Zhong-Xian; Wang, Jing-Xiu
Bibcode: 1987AcASn..28..111S
Altcode:
  The evolution of 300 quiet-region network features is followed in
  a time series of longitudinal magnetograms obtained (with spatial
  resolution 2-3 arcsec and time resolution about 2 h) using the VMG at
  Big Bear Solar Observatory on October 10-14, 1983. The results are
  presented in sample magnetograms and tables of numerical data. Four
  general evolution patterns are identified: (1) flux cancellation,
  (2) flux increase associated with the emergence of ephemeral regions,
  (3) one-polarity flux decrease, and (4) flux increase in one polarity
  without emergence of ephemeral regions. Patterns (3) and (4) are shown
  to be the dominant forms of decrease and increase, respectively.

Title: A comparison between hard X-ray, soft X-ray, and microwave
    images and H-alpha isophote map of the 1980 november 5 flare
Authors: Shi, Zhong-xian; Wang, Jing-xiu
Bibcode: 1987ChA&A..11..162S
Altcode:
  Filtergrams of the 1B/M1-M4 Hα flare of 1980 November 5 were digitized
  and the resulting isophote map compared with the hard X-, soft X,
  and microwave images. It was found: 1) During the first maximum. the
  high energy electrons did not penetrate the chromosphere. The Hα flare
  was probably caused by heat conduction from the (+7)-(+8) K hot plasma
  which generated the hard and soft X emissions. 2) The second maximum
  can be inferred to have been caused by bremsstrahlung of high energy
  electrons. The Hα maximum lagged behind the X-ray burst by not more
  than 5 seconds. 3) During the flash phase the area and the intensity
  of Hα emission increased in step with each other. 4) From the changes
  in the transverse magnetic field as outlined by Hα fibrils, (+31) ergs
  of magnetic energy is estimated to have been released in this flare.

Title: Fine structure and evolution of a subflare.
Authors: Shi, Z. -X.; Chen, J.; Wang, J. -X.
Bibcode: 1987PBeiO..10...69S
Altcode:
  No abstract at ADS

Title: The Evolution of Network Magnetic Fields of the Solar Quiet
    Regions
Authors: Shi, Z. X.; Wang, J. X.
Bibcode: 1987AcApS..28..119S
Altcode:
  No abstract at ADS

Title: The meteorites of Boxian and its minerals.
Authors: Wang, K. -R.; Wang, J. -X.; Li, X. -M.
Bibcode: 1987KexT...32..545W
Altcode:
  No abstract at ADS

Title: Do moving magnetic features represent sunspot decay?
Authors: Wang, J. -X.; Martin, S. F.; Livi, S. H. B.
Bibcode: 1987PBeiO..10...58W
Altcode:
  No abstract at ADS

Title: A comparison between hard X-ray, soft X-ray, microwave burst
    images and Hα isophote map of the flare on November 5, 1980.
Authors: Shi, Z. -X.; Wang, J. -X.
Bibcode: 1987ChJSS...7...18S
Altcode:
  No abstract at ADS

Title: On the propagation of magneto-acoustic-gravity waves
Authors: Wang, Jing-xiu
Bibcode: 1986ChA&A..10..291W
Altcode:
  An analysis of magneto-acoustic-gravity waves in the case of an
  isothermal atmosphere permeated by a uniform magnetic field is
  presented. The general solution is expressed in terms of generalized
  hypergeometric functions. It can be used in numerical simulation of
  oscillations in a magnetic atmosphere. It is shown that the elliptically
  polarized magneto-acoustic-gravity waves consist of a pair of surface
  waves and a pair of body waves above the cut-off frequency. The body
  waves along the magnetic field are similar to acoustic waves in an
  atmosphere and their cut-off frequency is unaffected by magnetic
  field. The transverse oscillation decreases with height. For the
  usual boundary condition, the longitudinal oscillation decreases with
  height; however, in some cases, it may contain terms that increase
  with height. The solution is singular on a family of ellipses in
  the frequency - horizontal wave number plane. Near these ellipses,
  the wave components grow indefinitely.

Title: On the propagation of magneto-acoustic-gravity waves
Authors: Wang, Jing-Xiu
Bibcode: 1986AcApS...6..231W
Altcode:
  An analysis of magnetoacoustic-gravity waves in the case of an
  isothermal atmosphere permeated by a uniform magnetic field is
  presented. The general solution is expressed in terms of generalized
  hypergeometric functions. It can be used in numerical simulation of
  oscillations in a magnetic atmosphere. It is shown that the elliptically
  polarized magnetoacoustic-gravity wave consist of a pair of surface
  waves and a pair of body waves above the cut-off frequency. The body
  waves along the magnetic field are similar to acoustic waves in an
  atmosphere, and their cut-off frequency is unaffected by magnetic
  field. The transverse oscillation decreases with height. For the
  usual boundary condition, the longitudinal oscillation decreases with
  height; however, in some cases, it may contain terms that increase
  with height. The solution is singular on a family of ellipses in
  the frequency - horizontal wave number plane. Near these ellipses,
  the wave components grow indefinitely.

Title: The Hα characteristics of hard X-ray bursts.
Authors: Shi, Zhong-Xian; Wang, Jing-Xiu
Bibcode: 1986ChJSS...6..243S
Altcode:
  The following results are obtained from the examination of 50 H-alpha
  flares. All flares with HXRBS are detectable from the emission of
  H-alpha + or - 2 A. They have at least two H-alpha kernels located in
  the opposite polarity regions. The H-alpha brightenings start earlier
  than HXRBS, while the H-alpha peaks, which correspond to the spikes of
  HXRBS very well, come later than that of HXRBS by several seconds. If
  the count rates of HXRBS are more than 1000, the kernels of H-alpha
  +2 A cover the penumbra; if the count rates are less than 200, the
  kernels do not cover the penumbra.

Title: The boundary value problem of the solar force-free magnetic
    field with constant α and its analytical solution
Authors: Chen, Z. -C.; Wang, J. -X.
Bibcode: 1986SoPh..103..317C
Altcode:
  In this paper we present a physical model which uses boundary
  conditions which seem to correspond more appropriately to actual
  situations. A boundary value problem of solar force-free magnetic
  field with constant α has been specified to represent the discretely
  concentrated characteristics of the longitudinal magnetic field on
  the photosphere. A unique analytical solution for the problem is
  obtained by a more strict method in mathematical physics. The most
  distinctive feature of our method is to make the solution be the
  superposition of the fields of single sources which are described by
  the physical parameters of corresponding sunspots on the photosphere,
  such as their position, strength, decay rates and the extent of the same
  polarity. The solution enables us to make an analytical description of
  the configuration of the magnetic field in the chromosphere and corona,
  and to investigate more conveniently its development as the foot points
  on the photosphere evolve.

Title: A unique solution for the boundary value problem of the solar
    force free magnetic field with constant α.
Authors: Chen, Z. -C.; Wang, J. -X.
Bibcode: 1985KexT...30..768C
Altcode:
  No abstract at ADS

Title: The oscillator strength of hydrogen lines
Authors: Shi, Zhong-xian; Wang, Jing-xiu
Bibcode: 1984ChA&A...8...94S
Altcode:
  We give a formal expression for the dependence of hydrogen line
  oscillator strength on departure from LTE and propose a method for
  determining this departure in the various sub-levels of the hydrogen
  atom in solar prominences. Results for 10 solar prominences are
  given. Finally, we discuss the possible implications of a smaller
  population in the 2p level than in the 2s level.

Title: A method of analysing the emission lines of solar prominences
Authors: Wang, Jing-xiu; Shi, Zhong-xian
Bibcode: 1983ChA&A...7..269W
Altcode:
  A new method of analysing the emission spectrum of solar prominences
  is presented, in which the source function is allowed to vary with
  optical depth. Least-squares fitting of the observed profile determines
  simultaneously the optical depth τ <SUB>0</SUB>, the Doppler width
  Δλ <SUB>D</SUB> and the factor α characterising the variation of the
  source function. This method is applied to the early Balmer lines in
  ten prominences of Ref. [1]. The results show that the source function
  of the self-reversed H <SUB>α</SUB> line increases towards the centre
  of the prominence, the value at the centre is 1.2-2.5 times the value
  at the edge. Neglect of this variation will give too large values
  of τ <SUB>0</SUB>. The degree of attenuation by selfabsorption also
  depends on this variation. Discussion of the variation gives support
  to the view that the main exciting mechanism in solar prominences is
  the scattering of the incident radiation.

Title: A method of analyzing the emission lines of solar prominences
Authors: Wang, J. -X.; Shi, Z. -X.
Bibcode: 1983AcApS...3..169W
Altcode:
  A new method of analyzing the emission spectrum of solar prominences
  is presented, in which the source function is allowed to vary with
  optical depth. Least-squares fitting of the observed profile determines
  simultaneously the optical depth T(0), the Doppler width, and the factor
  characterizing the variation of the source function. This method is
  applied to the early Balmer lines in ten prominences of Ye (1961). The
  results show that as the source function of the self-reversed H-alpha
  line increases towards the center of the prominence, the value at
  the center is 1.2 - 2.5 times the value at the edge. Neglect of this
  variation will give too large values of T(0). The degree of attenuation
  by self-absorption also depends on this variation. Discussion of the
  variation gives support to the view that the main exciting mechanism
  in solar prominences is the scattering of the incident radiation.

Title: The oscillator strength of hydrogen lines
Authors: Shi, Z. -X.; Wang, J. -X.
Bibcode: 1983AcApS...3..327S
Altcode:
  A formal expression is given for the dependence of hydrogen-line
  oscillator strength on departure form LTE, and a method is proposed for
  determining this departure in the various sublevels of the hydrogen
  atom in solar prominences. Results for 10 solar prominences are
  given. Finally, the possible implications of a smaller population in
  the 2p level than in the 2s level are discussed.

