Author name code: topka
ADS astronomy entries on 2022-09-14
author:"Topka, Kenneth P." 
------------------------------------------------------------------------  

Title: The Kepler Science Operations Center Pipeline: An Overview
    of Science Processing and Data Products
Authors: Jenkins, Jon Michael; Bryson, S. T.; Batalha, N. M.; Caldwell,
   D. A.; Borucki, W. J.; Koch, D. G.; Chandrasekaran, H.; Quintana,
   E. V.; Allen, C. L.; Pletcher, D. P.; Klaus, T.; Middour, C.; Girouard,
   F.; Wohler, W.; Cote, M.; McCauliff, S.; Bhavsar, P.; Topka, K.
Bibcode: 2007AAS...21113517J
Altcode: 2007BAAS...39..975J
  The Kepler Mission is designed to discover and characterize the
  frequency of Earth-size planets in the habitable zone of solar-like
  stars by observing 100,000 main-sequence stars in a 100 square degree
  field of view (FOV) for at least 3.5 years. The Kepler photometer will
  collect and transmit pixels of interest for target stars and associated
  collateral data which are received and processed by the Kepler Science
  Operations Center (SOC) located at NASA Ames Research Center. The
  data are reduced to produce flux time series for each target star,
  which are archived at the Data Management Center (DMC) located at
  STScI. Systematic errors are removed from each time series, which and
  are then subjected to searches for signatures of transiting planets
  and reflected light from close-in giant planets. A series of validation
  tests are automatically performed on the resulting threshold-crossing
  events to assist the science team in prioritizing the candidates for
  follow up observations. <P />Performing this level of processing on
  &gt;100,000 stars over a 3.5 year period is a significant challenge. The
  SOC Pipeline supports automated scheduling of the data reduction upon
  data arrival. We describe each data reduction step from initial pixel
  level calibrations to the extraction of photometric time series, to
  the detection of planetary signatures. We cover the architecture of
  the infrastructure supporting the science operations. The SOC Pipeline
  also supports the critical tasks of catalog and target management,
  as well as performing automated health and performance monitoring of
  the Kepler photometer in flight. <P />Funding for this mission provided
  by NASA's Discovery Program Office, SMD.

Title: Validation of Kepler Planet Candidates
Authors: Caldwell, Douglas A.; Batalha, N. M.; Borucki, W. J.; Koch,
   D. G.; Chandrasekaran, H.; Jenkins, J. M.; Topka, K. P.; Gautier,
   T. N.; Gilliland, R. L.
Bibcode: 2006AAS...20921013C
Altcode: 2006BAAS...38.1189C
  The Kepler Mission will be able to detect transiting Earth-size
  planets in the habitable zone of 30,000 stars and 1.4 Earth radius
  planets around 100,000 stars. Such sensitivity will allow Kepler
  to detect hundreds of terrestrial planets if they are common, or
  place significant upper limits on their numbers if they are rare. In
  addition, Kepler will detect many astrophysical false-positives that
  mimic transit signals. Most will be background eclipsing binaries
  as much as nine magnitudes fainter than the target star. We expect
  1000 background binaries with periods less than 3 days and 275 with
  longer periods. We have developed a series of automated tests on each
  detection, the results of which are used to decide whether planet
  candidates will be passed on for follow-up imaging and spectroscopic
  observations. <P />The validation process begins with model planet
  and eclipsing binary signal fits to the candidate detections. After
  subtracting the best-fit planet model, we search the residual flux
  time series for additional transiting planets around the star. This
  process is repeated until there are no new candidate detections. The
  candidate’s centroid time series is then tested against the model
  planet signal(s) in order to eliminate background eclipsing binaries
  through the change in photocenter position during the eclipse. For
  a 12<SUP>th</SUP> magnitude G2 star we can discriminate a binary
  mimicking an Earth transit if it is separated from the target star by
  a quarter of a pixel or more. Tests are also performed to see if the
  candidate signal is detected anomalously in only a single pixel of
  the aperture (e.g., a variable bad pixel), or if the signal is seen
  in the background estimate, or in any of the engineering data (e.g.,
  focal plane temperatures,). <P />Funding for Kepler is provided by
  NASA’s Discovery Program.

Title: Quick Look Software for the Kepler Photometer
Authors: Topka, Kenneth; Jenkins, J.; Caldwell, D.; Borucki, W. J.
Bibcode: 2006AAS...20921012T
Altcode: 2006BAAS...38.1189T
  Kepler is NASA’s first mission capable of finding extra-solar
  terrestrial planets that are Earth-size and smaller. The instrument
  includes a high gain antenna that is bolted in a fixed position on
  the satellite. Thus, the satellite will be rotated in order to point
  the antenna at Earth for transmission, an operation that will occur
  approximately once a month. In between Earth pointing communication
  with Kepler is also possible using a low gain antenna via X-band,
  normally used for up-link of commands and down-link of engineering
  data. Some of this band pass is reserved for pixel data as well, making
  limited amount of science data available for quick look analysis about
  twice a week. <P />Quick look software analyzes instrument health
  and performance as soon as possible after the data are obtained using
  the pixel data from X-band. The performance assessments are based on
  examination of time series data generated by the software, and include
  stellar brightness, centroid locations, plate scale, encircled energy,
  background flux values, CCD black, smear, and dark current levels,
  CCD dynamic range, and attitude solution. A more detailed analysis
  will be performed after the monthly down-link of all science data. New
  time series analyzed then include cosmic ray hit rate, CCD hot pixel
  formation rate, and combined differential photometric precision. All
  the metrics calculated for quick look will be reanalyzed at higher
  precision and higher time resolution. <P />The Kepler mission is funded
  by NASA’s Discovery Program

Title: Properties of the Smallest Solar Magnetic
    Elements. II. Observations versus Hot Wall Models of Faculae
Authors: Topka, K. P.; Tarbell, T. D.; Title, A. M.
Bibcode: 1997ApJ...484..479T
Altcode:
  Observations obtained at the Swedish Solar Observatory, La Palma,
  using the Lockheed tunable filter, have been used to measure
  properties of active region faculae, including contrast from disk
  center to near the limb. The data consist of coregistered digital
  photometric images of the line-of-sight magnetic field and of the
  continuum intensity. <P />The results are related to the structure
  of the individual flux tubes comprising faculae in active regions. In
  addition to center-limb contrast, the observations reveal a change in
  contrast between heliocentric angles of about 45° and 60° related
  to the ``turn-on'' of bright faculae. A class of models has been
  constructed that describes a facula as an evacuated thin flux tube
  with a hot wall and a depressed cool floor (hot wall model). The
  hot wall model is very successful in predicting the observations,
  including the changes observed between 45° and 60°. <P />The model
  predicts that the larger flux tubes comprising active region plage are
  micropores with a Wilson depression of 100 km largely independent of
  micropore diameter. Their typical diameter is 350-650 km; the largest
  ones are about 1200 km across. Bright points are the major component of
  active region plages by number, but micropores probably are the major
  component by total magnetic flux. Bright active region faculae seen
  near the limb are simply micropores viewed from the side, where the hot
  wall is visible and the depressed cool floor is not. The temperature
  difference between cool floor and hot wall varies from 300 to nearly
  500 K, depending on tube diameter and heliocentric angle. <P />These
  results have important implications for solar irradiance variations.

Title: Solar Irradiance Variations due to the Quiet Sun Network
Authors: Topka, K. P.; Tarbell, T. D.; Title, A. M.
Bibcode: 1997SPD....28.0263T
Altcode: 1997BAAS...29..904T
  An estimate for the change in total solar irradiance due to quiet sun
  network during the 11-year solar cycle is presented. The estimate is
  based on measurements of the center-limb contrast function for quiet
  sun magnetic elements. These measurements are the result of analysis
  of near-simultaneous, co-registered, digital, photometric images of
  the photospheric intensity (4300 - 6300 A) and line-of-sight magnetic
  field. Images were made with the Lockheed tunable filter instrument at
  the Swedish Solar Observatory, La Palma, between 1991 and 1994. The
  result is of order 0.1%. The images cover only a tiny fraction of
  the surface of the Sun and thus a very large extrapolation is made,
  limiting the accuracy of the result. Measurements made by satellite
  radiometers indicate that on the time scale of solar activity, the total
  solar irradiance is greater at activity maximum than at minimum by about
  0.1 to 0.15 %. Our result is consistent with this. Earlier results on
  active region plage, using similar data from La Palma, indicate that it
  does does not contribute significantly to long-term solar irradiance
  variations. This work has been supported by NSF contract ATM-9320353,
  by NASA contracts NASW-4612 and NAS8-39747, and by Lockheed IR funds.

Title: Solar Irradiance Variations due to Active Region Faculae
Authors: Topka, K. P.; Tarbell, T. D.; Title, A. M.
Bibcode: 1995SPD....26..512T
Altcode: 1995BAAS...27..959T
  No abstract at ADS

Title: Facular Contrast and Hot Wall Models of Flux Tubes
Authors: Topka, K. P.; Tarbell, T. D.; Title, A. M.
Bibcode: 1994AAS...185.8606T
Altcode: 1994BAAS...26.1465T
  Solar rotation causes features on its surface to be viewed at different
  angles. The appearance of active region faculae changes dramatically
  with viewing angle. They have minimum contrast at disk center, but
  appear bright near the limb. The nature of this center-limb variation
  is related to the structure of the individual flux tubes comprising
  faculae. One class of models depict a facula as an evacuated flux tube
  with hot walls and a depressed cool floor (hot wall model). Another
  depicts them as hot clouds, because of internal heating. Both can
  explain the observed center-limb variation in contrast. In this paper
  we ask whether there are other observable phenomena that can help
  differentiate between these models. The observations were obtained at
  the Swedish Solar Observatory, La Palma, using the Lockheed tunable
  filter. The data consist of co-registered images of line-of-sight
  magnetic field and of continuum intensity. The correlation between
  strong magnetic field and continuum intensity in active region faculae
  shows a remarkable and reproducible change between heliocentric angles
  of 50deg and 60deg . These results support the hot wall model, but not
  the hot cloud model. Hybrid models in which the flux tube has properties
  of both models cannot by ruled out. This work has been supported by
  NSF contract ATM-9320353, by NASA contracts NASW-4612 and NAS8-39747,
  and by Lockheed IR funds.

Title: Contrast of faculae near the disk center and solar variability
Authors: Lawrence, J. K.; Topka, K. P.; Jones, H. P.
Bibcode: 1993JGR....9818911L
Altcode:
  We analyze simultaneous, or near-simultaneous, coregistered, digital,
  photometric images of solar photospheric intensity and line-of-sight
  magnetic field. Images were made with the Lockheed tunable filter
  instrument at the Swedish Solar Observatory, La Palma, with the video
  spectra-spectroheliograph system at the San Fernando Observatory and
  with the new NASA spectromagnetograph at the National Solar Observatory
  at Kitt Peak. We study the disk center contrasts of small magnetic
  elements. While active region faculae are dark at disk center quiet
  Sun network features are bright. The populations of magnetic field
  elements that make up these two kinds of are quite different. Different
  contrast center-limb functions must be used when estimating their
  irradiance or luminosity contributions. The disk center contrasts of
  active region faculae are color dependent and indicate a depth effect
  related to the H<SUP>-</SUP> opacity of the facular atmosphere. This
  result is important for calibration of monochromatic observations
  of faculae to bolometric irradiance fluctuations. We emphasize the
  value of cooperative observations among installations whose differing
  strengths are complementary.

Title: The Quiet Sun Network and Solar Irradiance Variations
Authors: Topka, K. P.; Tarbell, T. D.; Title, A. M.
Bibcode: 1993BAAS...25R1183T
Altcode:
  No abstract at ADS

Title: La Palma Observations During the CoMStOC'92 Campaign
Authors: Shine, R.; Tarbell, T.; Topka, K.; Frank, Z.; Title, A.;
   Scharmer, G.
Bibcode: 1993BAAS...25S1223S
Altcode:
  No abstract at ADS

Title: Inclination of the Magnetic Lines-of-Force of Quiet Sun Network
Authors: Topka, K. P.; Tarball, T. D.; Title, A. M.; Lawrence, J.
Bibcode: 1993AAS...182.4803T
Altcode: 1993BAAS...25R.879T
  Photometric measurements of the continuum contrast of active region
  plage, after carefully removing all sunspots and pores, has been
  obtained for several years from the Swedish Solar Observatory, La
  Palma. More recently, similar measurements have been obtained for
  magnetic elements in the network far from active regions. These data
  were taken with the Lockheed tunable filter instrument using a CCD
  camera. The measurements indicate that at disk center active region
  plage is dark (negative contrast: intensity less than the surrounding
  quiet sun), while the network is bright. Furthermore, active region
  plage rapidly turns bright toward the limb; the network also brightens
  but more slowly. We have constructed a simple model that assumes
  that the magnetic lines-of-force are approximately vertical in active
  region plage, while those in the quiet sun network are inclined at the
  photosphere. This model correctly predicts the continuum contrast of
  network at disk center, and also its variation from center-to-limb. This
  provides evidence that the network is often inclined from vertical by
  30 degrees or more. This work was supported by Lockheed IR Funds, by
  NASA contracts NAS8-32805 (SOUP), NAS5-26813 (OSL), NAS5-30386 (MDI),
  and NAS8-38106 (BSOUP), and NSF contract ATM-8912841.

Title: ``The Active Sun'': Educational Videotapes on Solar Physics
    for College Astronomy
Authors: Hurlburt, N.; Title, A.; Tarbell, T.; Frank, Z.; Topka, K.;
   Shine, R.
Bibcode: 1993AAS...182.1002H
Altcode: 1993BAAS...25..809H
  We present a series of short, educational documentaries on solar
  physics aimed at college-level general astronomy courses. These
  tapes highlight recent advances in high-resolution solar astronomy
  and in theoretical and computational modeling of solar physics
  with particular focus on dynamical phenomena. The relevant physical
  mechanisms, theoretical interpretations and observational techniques
  are discussed. These include granulation, the theory of convection,
  five-minute oscillations, sunspots, magnetic fields, seeing and
  dopplergrams. VHS tapes are available to researchers and educators
  through a variety of distributors. This work supported by Lockheed
  Independent Research Funds.

Title: On the Magnetic and Velocity Field Geometry of Simple Sunspots
Authors: Title, Alan M.; Frank, Zoe A.; Shine, Richard A.; Tarbell,
   Theodore D.; Topka, Kenneth P.; Scharmer, Goran; Schmidt, Wolfgang
Bibcode: 1993ApJ...403..780T
Altcode:
  It is presently shown that a simple sunspot model with azimuthal
  variations in inclination, but lacking azimuthal field-strength
  variations, is free from azimuthal Lorentz forces. The meridional
  currents arising from the inclination variations are parallel to the
  field lines, suggesting that a cylindrically symmetric magnetostatic
  sunspot model can be perturbed into one with azimuthal variations in
  inclination with adjustment of the meridional force balance.

Title: White-light movies of the solar photosphere from the SOUP
    instrument on Spacelab 2 (Advances in Space Research 1986)
Authors: Title, A. M.; Tarbell, T. D.; Simon, G. W.; Acton, L.;
   Duncan, D.; Ferguson, S.; Finch, M.; Frank, Z.; Kelly, G.; Lindgren,
   R.; Morrill, M.; Pope, T.; Reeves, R.; Rehse, R.; Shine, R.; Topka,
   K.; Harvey, J.; Leibacher, J.; Livingston, W.; November, L.
Bibcode: 1993inas.book..100T
Altcode:
  No abstract at ADS

Title: Properties of the Smallest Solar Magnetic Elements. I. Facular
    Contrast near Sun Center
Authors: Topka, K. P.; Tarbell, T. D.; Title, A. M.
Bibcode: 1992ApJ...396..351T
Altcode:
  Measurements are presented which indicate that the continuum intensity
  of facular areas in solar active regions, outside sunspots and pores, is
  less than that of the quiet sun very near disk center. It is shown that
  the observed continuum intensity of faculae at disk center near 5000
  A is nearly 3 percent less than that of the quiet sun. The continuum
  contrast increases rapidly away from disk center, reaching +2 percent
  at 45 deg. The zero-crossing point, where the contrast changes sign,
  occurs at 20-degree heliocentric angle. This is contrary to many earlier
  observations. The constraint these observations place on the size
  of flux tubes depends upon the value of the zero-crossing point. It
  is proposed that most of the flux tubes in solar faculae may be very
  small, in the range 50-100 km in diameter, and that inclination from
  local vertical of about 10 deg at the photosphere is common on the
  sun. Footpoints of opposite polarity tend to tilt toward one another.

Title: Comparison of Active Region Facular Contrast Measurements to
    Simple Models
Authors: Topka, K. P.; Title, A. M.
Bibcode: 1992AAS...181.8104T
Altcode: 1992BAAS...24.1252T
  No abstract at ADS

Title: On the Differences between Plage and Quiet Sun in the Solar
    Photosphere
Authors: Title, Alan M.; Topka, Kenneth P.; Tarbell, Theodore D.;
   Schmidt, Wolfgang; Balke, Christiaan; Scharmer, Goran
Bibcode: 1992ApJ...393..782T
Altcode:
  Time sequences of interleaved observations of the continuum intensity,
  longitudinal magnetic field, vertical velocity in the midphotosphere,
  and the line-center intensity in Ni I 6768 A were obtained in an
  active-region plage and the surrounding relatively field-free area near
  disk center. Spacetime Fourier filtering techniques are used to separate
  the convective and oscillatory components of the solar atmosphere. The
  properties of the photosphere are found to differ qualitatively and
  quantitatively between the plage, where the field is 150 G or more,
  and its quiet surroundings. The scale of granulation is smaller, the
  contrast lower, and the temporal evolution slower in the plage than the
  quiet sun. In the plage, the vertical velocity is reduced in amplitude
  compared to the quiet sun, and there is little evidence of a granulation
  pattern, while in the quiet sun the vertical flow pattern is similar in
  size and shape to the underlying granulation pattern in the continuum.

Title: Facular Contrast Near Solar Disk Center and the Inclination
    of Magnetic Lines of Force from Local Vertical
Authors: Topka, K. P.; Tarbell, T. D.; Title, A. M.
Bibcode: 1992AAS...180.4004T
Altcode: 1992BAAS...24..793T
  No abstract at ADS

Title: High resolution observations: the state of the art and beyond.
Authors: Title, A.; Tarbell, T.; Shine, R.; Topka, K.; Frank, Z.
Bibcode: 1992ESASP.344....9T
Altcode: 1992spai.rept....9T
  Excellent telescopes on excellent sites with fast digital CCD cameras
  and special purpose computers allow the collection of broad band images
  at just the instants of good seeing. This has resulted in nearly optimal
  movies of the solar surface for several hours. When longer exposures
  are required for narrowband filtergrams or spectra it is not enough to
  capture single images. However, big fast memories allow the collection
  of many selected low signal-to-noise ratio images in real time, which
  can be summed to achieve the desired signal to noise ratios. Adaptive
  optics shows promise of diffraction limited images for limited fields
  of view. Nevertheless, groundbased observations will always be limited
  in their duration, uniformity, and resolution qualities which are
  essential for understanding the development and evolution of small scale
  processes. Until there are observations in space we will not be able
  to completely understand either the processes in the solar atmosphere
  or how processes occurring at different height are interrelated.

Title: Investigation of solar active regions at high resolution
    by balloon flights of the solar optical universal polarimeter,
    definition phase
Authors: Tarbell, Theodore D.; Topka, Kenneth P.
Bibcode: 1992lock.reptQ....T
Altcode:
  The definition phase of a scientific study of active regions on the sun
  by balloon flight of a former Spacelab instrument, the Solar Optical
  Universal Polarimeter (SOUP) is described. SOUP is an optical telescope
  with image stabilization, tunable filter and various cameras. After
  the flight phase of the program was cancelled due to budgetary
  problems, scientific and engineering studies relevant to future balloon
  experiments of this type were completed. High resolution observations
  of the sun were obtained using SOUP components at the Swedish Solar
  Observatory in the Canary Islands. These were analyzed and published
  in studies of solar magnetic fields and active regions. In addition,
  testing of low-voltage piezoelectric transducers was performed,
  which showed they were appropriate for use in image stabilization on
  a balloon.

Title: High Resolution Observations of the Magnetic and Velocity
    Field of Simple Sunspots
Authors: Title, Alan M.; Frank, Zoe A.; Shine, Richard A.; Tarbell,
   T. D.; Topka, K. P.; Scharmer, Goran; Schmidt, Wolfgang
Bibcode: 1992ASIC..375..195T
Altcode: 1992sto..work..195T
  We have observed the disk passage of relatively simple round sunspots
  using a narrowband filter and a large format CCD detector and have
  created magnetograms, Dopplergrams, and continuum images nearly
  simultaneously. In addition the spectral resolution of the filter
  allows the construction of 'spectra' for all points in the field of
  view. The mean inclination of the magnetic field increases from 45-50
  deg to 70-75 deg across the penumbra and there is a fluctuation of the
  inclination angle about the mean of about 4 +/- 18 deg. The variation in
  inclination is large enough that substantial amounts of magnetic field
  are parallel to the solar surface from the mid to outer penumbra. The
  Evershed flow tends to occur in the regions where the magnetic field
  is horizontal. This suggests that the Evershed flow is confined to the
  regions of horizontal fields. We show that a simple sunspot model with
  azimuthal variations in inclination but no azimuthal variations of
  field strength is free from azimuthal Lorentz forces. The meridional
  component of the currents which arise from the azimuthal variation
  in inclination are parallel to the field lines. This suggests that a
  cylindrically symmetric magnetostatic sunspot model can be perturbed
  into one with azimuthal variations in inclination with some adjustment
  in the meridional force balance.

Title: Low-Cost Space Missions in Solar Physics or Astrophysics
    Using Mass-Produced Spacecraft
Authors: Tarbell, T. D.; Jurcevich, B. K.; Title, A. M.; Topka, K. P.
Bibcode: 1991BAAS...23.1317T
Altcode:
  No abstract at ADS

Title: Properties of the Smallest Magnetic Elements on the Sun
Authors: Topka, K. P.; Smith, K. L.; Tarbell, T. D.; Title, A. M.;
   Scharmer, G.
Bibcode: 1991BAAS...23.1388T
Altcode:
  No abstract at ADS

Title: Power Spectra of Flows and Magnetic Fields in the Solar
    Photosphere
Authors: Tarbell, T. D.; Slater, G. L.; Frank, Z. A.; Topka, K. P.;
   Scharmer, G.; Schmidt, W.
Bibcode: 1991BAAS...23.1048T
Altcode:
  No abstract at ADS

Title: Sunspot Umbral and Penumbral Oscillations in Hα
Authors: Shine, R.; Tarbell, T.; Title, A.; Topka, K.; Frank, Z.;
   Smith, K.
Bibcode: 1991BAAS...23.1033S
Altcode:
  No abstract at ADS

Title: Stokes Polarimetry of a Sunspot from the Swedish Solar
    Observatory at La Palma
Authors: Topka, K. P.; Frank, Z. A.; Tarbell, T. D.; Title, A. M.;
   Scharmer, G.
Bibcode: 1991BAAS...23Q1052T
Altcode:
  No abstract at ADS

Title: High-resolution observations of the solar granulation.
Authors: Topka, K. P.; Title, A. M.
Bibcode: 1991sia..book..727T
Altcode:
  The opportunity to observe the solar surface from space and from
  excellent groundbased sites, combined with enhanced digital image
  recording and computer technology, has led to improved high-resolution
  observations of solar granulation in the last decade. Today, granulation
  movies over 1 hr long are available with spatial resolution of nearly
  1/3″(=240 km on the solar surface). These new data have modified our
  conception of solar granulation by showing it to be a more complicated
  combination of different phenomena than was previously appreciated. The
  smaller granules, for example, may be the result of the fragmentation
  of larger granules due to turbulent small-scale flows. The new data
  have been used to detect large-scale horizontal flows on the Sun's
  surface, by the direct measurement of the proper motion of granules
  during their lifetimes. These new results may also have important
  implications for the heating of the solar chromosphere and corona.

Title: Generation of Electric Currents and Waves on Magnetic Flux
    Tubes by Horizontal Velocities in the Photosphere (With 1 Figure)
Authors: Tarbell, T. D.; Slater, G. L.; Frank, Z. A.; Shine, R. A.;
   Topka, K. P.
Bibcode: 1991mcch.conf...39T
Altcode:
  No abstract at ADS

Title: SOUP Observations of Solar Activity
Authors: Shine, R. A.; Scharmer, G.; Tarbell, T. D.; Title, A. M.;
   Topka, K. P.
Bibcode: 1991max..conf..295S
Altcode:
  No abstract at ADS

Title: Detailed Comparison of Quiet and Magnetic Sun
Authors: Topka, K.; Ferguson, S.; Shine, R.; Tarbell, T.; Title, A.;
   Balke, C.; Scharmer, G.; Schmidt, W.
Bibcode: 1990BAAS...22R.879T
Altcode:
  No abstract at ADS

Title: Intermittency of Fine Scale Solar Magnetic Fields in the
    Photosphere
Authors: Tarbell, T.; Acton, S.; Topka, K.; Title, A.; Schmidt, W.;
   Scharmer, G.
Bibcode: 1990BAAS...22..878T
Altcode:
  No abstract at ADS

Title: Generation of Waves and Electric Currents on Magnetic Flux
    Tubes by Horizontal and Vertical Velocities in the Photosphere
Authors: Frank, Z. A.; Shine, R. A.; Slater, G.; Tarbell, T.; Topka, K.
Bibcode: 1990BAAS...22..878F
Altcode:
  No abstract at ADS

Title: Magnetic flux tubes and their relation to continuum and
    photospheric features
Authors: Title, A.; Tarbell, T.; Topka, K.; Cauffman, D.; Balke, C.;
   Scharmer, G.
Bibcode: 1990GMS....58..171T
Altcode:
  An investigation is made of the relationship between photospheric
  'filigree' light points, line-center brightness, and magnetic field,
  as inferred from sets of individual images and films showing a distinct
  difference between two classes of magnetic regions. While in the first
  such region the vertical velocity field is average and the magnetic
  field is mostly confined in narrow lanes, the granulation pattern
  of the second scale is much smaller, the vertical velocity is lower,
  and the magnetic field is less compact. Where granulation is normal,
  excellent correlation is obtained between bright continuum, line-center,
  and magnetic field line structure.

Title: High-Resolution Observations of Emerging Magnetic Fields and
    Flux Tubes in Active Region Photosphere
Authors: Tarbell, T.; Ferguson, S.; Frank, Z.; Shine, R.; Title, A.;
   Topka, K.; Scharmer, G.
Bibcode: 1990IAUS..138..147T
Altcode:
  No abstract at ADS

Title: High Resolution Observations of the Photosphere
Authors: Title, A. M.; Shine, R. A.; Tarbell, T. D.; Topka, K. P.;
   Scharmer, G. B.
Bibcode: 1990IAUS..138...49T
Altcode:
  No abstract at ADS

Title: Intial Results of the Lockheed 1989 La Palma Observing Campaign
Authors: Topka, K.; Frank, Z.; Shine, R.; Smith, K.; Tarbell, T.;
   Title, A.; Scharmer, G.
Bibcode: 1989BAAS...21.1111T
Altcode:
  No abstract at ADS

Title: High - resolution observations of emerging magnetic flux
Authors: Tarbell, T. D.; Topka, K.; Ferguson, S.; Frank, Z.; Title,
   A. M.
Bibcode: 1989hsrs.conf..506T
Altcode:
  No abstract at ADS

Title: Variation of granulation properties on a meso-granular scale
Authors: Brandt, P. N.; Ferguson, S.; Scharmer, G. B.; Shine, R. A.;
   Tarbell, T. D.; Title, A. M.; Topka, K.
Bibcode: 1989hsrs.conf..473B
Altcode:
  No abstract at ADS

Title: Proper Motion and Lifetime of Mesogranules
Authors: Frank, Z.; Muller, R.; Roudier, T.; Vigneau, J.; Shine, R.;
   Tarbell, T.; Title, A.; Topka, K.; Simon, G.
Bibcode: 1989BAAS...21..841F
Altcode:
  No abstract at ADS

Title: Short Term Evolution of Fine Scale Magnetic Structures
Authors: Topka, K.; Frank, Z.; Shine, R.; Tarbell, T.; Title, A.;
   Scharmer, G.; Balke, A.
Bibcode: 1989BAAS...21..842T
Altcode:
  No abstract at ADS

Title: Investigation of Active Regions at High Resolution by Balloon
    Flights of the Solar Optical Universal Polarimeter (SOUP)
Authors: Tarbell, T.; Gilbreth, C.; Shine, R.; Title, A.; Topka, K.;
   Wolfson, J.
Bibcode: 1989BAAS...21R.837T
Altcode:
  No abstract at ADS

Title: Observations of Running Penumbral Waves
Authors: Shine, R.; Tarbell, T.; Title, A.; Topka, K.; Frank, Z.;
   Scharmer, G.
Bibcode: 1989BAAS...21..837S
Altcode:
  No abstract at ADS

Title: Details of Large Scale Solar Motions Revealed by Granulation
    Test Particles
Authors: Simon, G. W.; November, L. J.; Ferguson, S. H.; Shine, R. A.;
   Tarbell, T. D.; Title, A. M.; Topka, K. P.; Zirin, H.
Bibcode: 1989ASIC..263..371S
Altcode: 1989ssg..conf..371S
  No abstract at ADS

Title: Statistical Properties of Solar Granulation Derived from the
    SOUP Instrument on Spacelab 2
Authors: Title, A. M.; Tarbell, T. D.; Topka, K. P.; Ferguson, S. H.;
   Shine, R. A.; SOUP Team
Bibcode: 1989ApJ...336..475T
Altcode:
  Computer algorithms and statistical techniques were used to identify,
  measure, and quantify the properties of solar granulation derived
  from movies collected by the Solar Optical Universal Polarimeter on
  Spacelab 2. The results show that there is neither a typical solar
  granule nor a typical granule evolution. A granule's evolution is
  dependent on local magnetic flux density, its position with respect to
  the active region plage, its position in the mesogranulation pattern,
  and the evolution of granules in its immediate neighborhood.

Title: Flows, Random Motions and Oscillations in Solar Granulation
    Derived from the SOUP Instrument on Spacelab 2
Authors: Title, A. M.; Tarbell, T. D.; Topka, K. P.; Ferguson, S. H.;
   Shine, R. A.; SOUP Team
Bibcode: 1989ASIC..263..225T
Altcode: 1989ssg..conf..225T
  No abstract at ADS

Title: Magnetoconvection on the solar surface.
Authors: Simon, G. W.; Title, A. M.; Topka, K. P.; Tarbell, T. D.;
   Shine, R. A.; Ferguson, S. H.; Zirin, H.
Bibcode: 1989GMS....54...53S
Altcode: 1989sspp.conf...53S
  The authors describe and illustrate the first high-resolution
  observations of horizontal flows on the solar surface and their relation
  to magnetic field structure seen in the Sun's photosphere.

Title: Investigation of active regions at high resolution by balloon
    flights of the Solar Optical Universal Polarimeter (SOUP)
Authors: Tarbell, T.; Frank, Z.; Gilbreth, C.; Shine, R.; Title, A.;
   Topka, K.; Wolfson, J.
Bibcode: 1989dots.work..310T
Altcode:
  SOUP is a versatile, visible-light solar observatory, built for space
  or balloon flight. It is designed to study magnetic and velocity
  fields in the solar atmosphere with high spatial resolution and
  temporal uniformity, which cannot be achieved from the surface of the
  earth. The SOUP investigation is carried out by the Lockheed Palo Alto
  Research Laboratory, under contract to NASA's Marshall Space Flight
  Center. Co-investigators include staff members at a dozen observatories
  and universities in the U.S. and Europe. The primary objectives of the
  SOUP experiment are: to measure vector magnetic and velocity fields in
  the solar atmosphere with much better spatial resolution than can be
  achieved from the ground; to study the physical processes that store
  magnetic energy in active regions and the conditions that trigger
  its release; and to understand how magnetic flux emerges, evolves,
  combines, and disappears on spatial scales of 400 to 100,000 km. SOUP
  is designed to study intensity, magnetic, and velocity fields in the
  photosphere and low chromosphere with 0.5 arcsec resolution, free of
  atmospheric disturbances. The instrument includes: a 30 cm Cassegrain
  telescope; an active mirror for image stabilization; broadband film
  and TV cameras; a birefringent filter, tunable over 5100 to 6600 A
  with 0.05 A bandpass; a 35 mm film camera and a digital CCD camera
  behind the filter; and a high-speed digital image processor.

Title: High-resolution digital movies of emerging flux and horizontal
    flows in active regions on the sun
Authors: Topka, K.; Ferguson, S.; Frank, Z.; Tarbell, T.; Title, A.
Bibcode: 1988fnsm.work..283T
Altcode:
  High-resolution observations of active regions in many wavelength bands
  obtained at the Vacuum Tower Telescope of NSO/Sunspot (Sacramento Peak)
  are presented. The SOUP tunable filter, HRSO 1024 x 1024 CCD camera,
  and a sunspot tracker for image stabilization were used. Subarrays of
  512 x 512 pixels were processed digitally and recorded on videodisk
  in movie format. The movies with 0.5 to 1 arcsecond resolution of
  the following simultaneous observations were shown: green continuum,
  longitudinal magnetogram, Doppler velocity, Fe I 5576 A line center,
  H alpha wings, and H alpha line center. The best set of movies show a
  90 x 90 arcsecond field-of-view of an active region at S29, W11. When
  viewed at speeds of a few thousand times real-time, the photospheric
  movies clearly show the active region fields being distorted by a
  remarkable combination of systematic flows and small eruptions of new
  flux. Flux emergence is most easily discovered in line center movies:
  an elongated dark feature appears first, followed soon after by bright
  points at one or both ends. A brief, strong upflow is seen when the
  dark feature first appears; downflow in the bright points persists
  much longer. The magnetic flux appears to increase gradually over this
  extended period. Some of the flux emergence events were studied in
  detail, with measurements of horizontal and vertical velocities and
  magnetic flux versus time within one footpoint of the loop.

Title: Statistical properties of solar granulation from the SOUP
    instrument on Spacelab 2
Authors: Topka, K.; Title, A.; Tarbell, T.; Ferguson, S.; Shine, R.
Bibcode: 1988fnsm.work..294T
Altcode:
  The Solar Optical Universal Polarimeter (SOUP) on Spacelab 2 collected
  movies of solar granulation completely free from atmospheric blurring,
  and are not degraded by pointint jitter (the pointing stability
  was 0.003 sec root mean square). The movies illustrate that the
  solar five minute oscillation has a major role in the appearance of
  solar granulation and that exploding granules are a common feature
  of the granule evolution. Using 3-D Fourier filtering techniques
  the oscillations were removed and it was demonstrated that the
  autocorrelation lifetime of granulation is a factor of two greater
  in magnetic field regions than in field-free quiet sun. Horizontal
  velocities were measured and flow patterns were observed on the scale of
  meso- and super granulation. In quiet regions the mean flow velocity
  is 370 m/s while in the magnetic regions it is about 125 m/s. It
  was also found that the root mean square (RMS) fluctuating horizonal
  velocity field is substantially greater in quiet sun than in strong
  magnetic field regions. By superimposing the location of exploding
  granules on the average flow maps it was found that they appear almost
  exclusively in the center of mesogranulation size flow cells. Because
  of the nonuniformity of the distribution of exploding granules, the
  evolution of the granulation pattern in mesogranule cell centers and
  boundaries differs fundamentally. It is clear from this study there
  is neither a typical granule nor a typical granule evolution.

Title: Observations of photospheric magnetic fields and shear flows
    in flaring active regions
Authors: Tarbell, T.; Ferguson, S.; Frank, Z.; Title, A.; Topka, K.
Bibcode: 1988fnsm.work...50T
Altcode:
  Horizontal flows in the photosphere and subsurface convection zone move
  the footpoints of coronal magnetic field lines. Magnetic energy to power
  flares can be stored in the corona if the flows drive the fields far
  from the potential configuration. Videodisk movies were shown with 0.5
  to 1 arcsecond resolution of the following simultaneous observations:
  green continuum, longitudinal magnetogram, Fe I 5576 A line center
  (mid-photosphere), H alpha wings, and H alpha line center. The movies
  show a 90 x 90 arcsecond field of view of an active region at S29,
  W11. When viewed at speeds of a few thousand times real-time, the
  photospheric movies clearly show the active region fields being
  distorted by a remarkable combination of systematic flows and small
  eruptions of new flux. Magnetic bipoles are emerging over a large area,
  and the polarities are systematically flowing apart. The horizontal
  flows were mapped in detail from the continuum movies, and these may
  be used to predict the future evolution of the region. The horizontal
  flows are not discernable in H alpha. The H alpha movies strongly
  suggest reconnection processes in the fibrils joining opposite
  polarities. When viewed in combination with the magnetic movies,
  the cause for this evolution is apparent: opposite polarity fields
  collide and partially cancel, and the fibrils reconnect above the
  surface. This type of reconnection, driven by subphotospheric flows,
  complicates the chromospheric and coronal fields, causing visible
  braiding and twisting of the fibrils. Some of the transient emission
  events in the fibrils and adjacent plage may also be related.

Title: Observations of Granulation in Quiet and Magnetic Sun from
    the Swedish Solar Observatory on LaPalma
Authors: Topka, K.; Ferguson, S.; Frank, Z.; Shine, R.; Tarbell, T.;
   Title, A.; Wolfson, J.; Scharmer, G.; Brandt, P.
Bibcode: 1988BAAS...20S1010T
Altcode:
  No abstract at ADS

Title: Solar Activity and Flare Observations from the Swedish Solar
    Observatory on La Palma
Authors: Wolfson, J.; Ferguson, S.; Frank, Z.; Shine, R.; Tarbell,
   T.; Title, A.; Topka, K.; Scharmer, G.; Brandt, P.; Gurman, J.
Bibcode: 1988BAAS...20..978W
Altcode:
  No abstract at ADS

Title: On the Relation between Photospheric Flow Fields and the
    Magnetic Field Distribution on the Solar Surface
Authors: Simon, George W.; Title, A. M.; Topka, K. P.; Tarbell, T. D.;
   Shine, R. A.; Ferguson, S. H.; Zirin, H.; SOUP Team
Bibcode: 1988ApJ...327..964S
Altcode:
  Using the technique of local correlation tracking on a 28 minute time
  sequence of white-light images of solar granulation, the horizontal
  flow field on the solar surface is measured. The time series was
  obtained by the Solar Optical Universal Polarimeter (SOUP) on Spacelab 2
  (Space Shuttle flight 51-F) and is free from atmospheric blurring and
  distortion. The SOUP flow fields have been compared with carefully
  aligned magnetograms taken over a nine hour period at the Big Bear
  Solar Observatory before, during, and after the SOUP images. The flow
  field and the magnetic field agree in considerable detail: vectors which
  define the flow of the white-light intensity pattern (granulation) point
  toward magnetic field regions, magnetic fields surround flow cells, and
  magnetic features move along the flow arrows. The projected locations
  of free particles ('corks') in the measured flow field congregate at
  the same locations where the magnetic field is observed.

Title: Observations of Photospheric Magnetic Fields and Shear Flows
    in Flaring Active Regions
Authors: Tarbell, T.; Ferguson, S.; Frank, Z.; Title, A.; Topka, K.
Bibcode: 1988BAAS...20..744T
Altcode:
  No abstract at ADS

Title: High-Resolution Digital Movies of Emerging Flux and Horizontal
    Flows in Active Regions on the Sun
Authors: Tarbell, T.; Ferguson, S.; Frank, Z.; Title, A.; Topka, K.
Bibcode: 1988BAAS...20..680T
Altcode:
  No abstract at ADS

Title: Statistical Properties of Solar Granulation from the SOUP
    Instrument on Spacelab 2
Authors: Topka, K.; Title, A.; Tarbell, T.; Ferguson, S.; Shine, R.
Bibcode: 1988BAAS...20Q.679T
Altcode:
  No abstract at ADS

Title: Variability of solar mesogranulation
Authors: Simon, G. W.; November, L. J.; Acton, L. W.; Ferguson, S. H.;
   Shine, R. A.; Tarbell, T. D.; Title, A. M.; Topka, K. P.; Zirin, H.
Bibcode: 1988AdSpR...8g.169S
Altcode: 1988AdSpR...8..169S
  From white-light photographs of solar granulation obtained with the
  SOUP instrument on Space Shuttle Flight STS-19 we have measured the
  motions of granules using local correlation tracking techniques. The
  granules are organized into larger-scale structures (mesogranular and
  supergranular) which exhibit outflow from upwellings, convergence into
  sinks, as well as significant vorticity. Magnetic fields follow these
  same flow patterns. We describe these velocity structures, and suggest
  that their effect on magnetic field structures may be important to
  the solar flare buildup process.

Title: Correlation Lifetimes of Quiet and Magnetic Granulation from
    the SOUP Instrument on Spacelab 2
Authors: Title, A.; Tarbell, T.; Topka, K.; Acton, L.; Duncan, D.;
   Ferguson, S.; Finch, M.; Frank, Z.; Kelly, G.; Lindgren, R.; Morrill,
   M.; Pope, T.; Reeves, R.; Rehse, R.; Shine, R.; Simon, G.; Harvey,
   J.; Leibacher, J.; Livingston, W.; November, L.; Zirker, J.
Bibcode: 1988ApL&C..27..141T
Altcode:
  The time sequences of diffraction limited granulation images obtained by
  the Solar Optical Universal Polarimeter on Spacelab 2 are presented. The
  uncorrection autocorrelation limetime in magnetic regions is dominated
  by the 5-min oscillation. The removal of this oscillation causes the
  autocorrelation lifetime to increase by more than a factor of 2. The
  results suggest that a significant fraction of granule lifetimes are
  terminated by nearby explosions. Horizontal displacements and transverse
  velocities in the intensity field are measured. Lower limits to the
  lifetime in the quiet and magnetic sun are set at 440 s and 950 s,
  respectively.

Title: The relation between convection flows and magnetic structure
    at the solar surface
Authors: Simon, G. W.; November, L. J.; Acton, L. W.; Title, A. M.;
   Tarbell, T. D.; Topka, K. P.; Shine, R. A.; Ferguson, S. H.; Weiss,
   N. O.; Zirin, H.
Bibcode: 1988AdSpR...8k.133S
Altcode: 1988AdSpR...8..133S
  We describe recent results from the comparison of data from the Solar
  Optical Universal Polarimeter instrument on Spacelab 2 and magnetograms
  from Big Bear Solar Observatory. We show that the Sun's surface velocity
  field governs the structure of the observed magnetic field over the
  entire solar surface outside sunspots and pores. We attempt to describe
  the observed flows by a simple axisymmetric plume model. Finally,
  we suggest that these observations may have important implications
  for the prediction of solar flares, mass ejections, and coronal heating.

Title: White Light Sunspot Observations from the Solar Optical
    Universal Polarimeter on Spacelab-2
Authors: Shine, R. A.; Title, A. M.; Tarbell, T. D.; Topka, K. P.
Bibcode: 1987Sci...238.1264S
Altcode:
  The flight of the Solar Optical Universal Polarimeter on Spacelab-2
  provided the opportunity for the collection of time sequences of
  diffraction-limited (0.5 arc second) solar images with excellent
  pointing stability (0.003 arc second) and with freedom from the
  distortion that plagues ground-based images. A series of white-light
  images of active region 4682 were obtained on 5 August 1985, and
  the area containing the sunspot has been analyzed. These data have
  been digitally processed to remove noise and to separate waves from
  low-velocity material motions. The results include (i) proper motion
  measurements of a radial outflow in the photospheric granulation
  pattern just outside the penumbra; (ii) discovery of occasional bright
  structures (``streakers'') that appear to be ejected outward from the
  penumbra; (iii) broad dark ``clouds'' moving outward in the penumbra,
  in addition to the well-known bright penumbral grains moving inward;
  (iv) apparent extensions and contractions of penumbral filaments over
  the photosphere; and (v) observation of a faint bubble or looplike
  structure that seems to expand from two bright penumbral filaments
  into the photosphere.

Title: High-Resolution CCD Observations of Doppler and Magnetic
    Images in the Solar Photosphere
Authors: Tarbell, T. D.; Frank, Z. A.; Morrill, M. E.; Shine, R. A.;
   Topka, K. P.; Title, A. M.
Bibcode: 1987BAAS...19.1117T
Altcode:
  No abstract at ADS

Title: On the Relation between Magnetic Field Structures and
    Granulation
Authors: Title, A. M.; Tarbell, T. D.; Topka, K. P.
Bibcode: 1987ApJ...317..892T
Altcode:
  Narrow-band observations of a solar emerging-flux region, obtained
  at 525.02 nm with resolution 0.5 arcsec using the Sacramento Peak
  vacuum-tower telescope and the Spacelab 2 tunable filter on December
  10, 1979, are reported. The data are presented in histograms and
  characterized in detail. Magnetic-flux concentrations of 600-1000 G
  are found to be located in areas of suppressed downflow near holes or
  pores in the granulation pattern, while 100-500-G concentrations occur
  in areas with stronger downdrafts, in cell-like structures of diameter
  2-5 arcsec, the fields being aligned with dark intergranular lanes. It
  is inferred that granulation concentrates the magnetic field in the
  downflow lanes (as found in numerical simulations by Nordlund, 1983),
  and that the magnetic structures are more diffuse and longer-lasting
  than the bright spots; thus bright-point maps are contained in, rather
  than equivalent to, magnetic-field maps.

Title: On the Relation Between Large-Scale Granular Flows and
    Supergranules and Mesogranules
Authors: Simon, G.; Ferguson, S.; Tarbell, T.; Title, A.; Topka, K.;
   November, L.; Zirin, H.
Bibcode: 1987BAAS...19R.935S
Altcode:
  No abstract at ADS

Title: Simultaneous Observations of Emerging Flux from the Big Bear
    Solar Observatory and the SOUP Instrument on Spacelab 2
Authors: Topka, K.; Ferguson, S.; Title, A.; Tarbell, T.; Zirin, H.;
   Simon, G.; November, L.
Bibcode: 1987BAAS...19R.927T
Altcode:
  No abstract at ADS

Title: Simultaneous Sunspot Observations from the SOUP Instrument
    on Spacelab 2 and the Big Bear Solar Observatory
Authors: Shine, R. A.; Title, A. M.; Topka, K. P.; Tarbell, T. D.;
   Zirin, H.
Bibcode: 1987BAAS...19..927S
Altcode:
  No abstract at ADS

Title: Exploding and Elongated Granules
Authors: Title, A. M.; Tarbell, T. D.; Ferguson, S. H.; Topka, K. P.
Bibcode: 1987BAAS...19Q.927T
Altcode:
  No abstract at ADS

Title: New Ideas About Granulation Based on Data from the Solar
    Optical Universal Polarimeter Instrument on Spacelab 2 and Magnetic
    Data from Big Bear Solar Observatory
Authors: Title, A. M.; Tarbell, T. D.; Topka, K. P.; Shine, R. A.;
   Simon, G. W.; Zirin, H.; SOUP Team
Bibcode: 1987LNP...292..173T
Altcode: 1987ssp..conf..173T
  The SOUP flow fields have been compared with carefully aligned
  magnetograms taken at the BBSO before, during, and after the SOUP
  images. The magnetic field is observed to exist in locations where
  either the flow is convergent or on the boundaries of the outflow from
  a flow cell center. Streamlines calculated from the flow field agree
  very well with the observed motions of the magnetic field in the BBSO
  magnetogram movies.

Title: High-Resolution Observations of Changing Magnetic Features
    on the Sun
Authors: Topka, K. P.; Tarbell, T. D.; Title, A. M.
Bibcode: 1986ApJ...306..304T
Altcode:
  The total magnetic flux present in 28 small isolated unipolar features
  that surround an active region has been measured on a well-registered
  sequence of high-resolution magnetograms. Seventeen features showed no
  changes, but the rest showed changes in measured flux with time that
  were much greater than the uncertainty in the flux determination. Two
  magnetic features showed evidence for increases in flux with time,
  while nine others showed decay. In some cases the decaying features
  appear to be canceling with nearby opposite polarity flux, which may
  represent the submergence of flux below the photosphere. In others,
  the observed decay occurs in regions that are strictly unipolar,
  with no observable opposite polarity flux present. Some evidence for
  the outward diffusion of flux from a decaying feature in a unipolar
  region was found.

Title: Properties of Solar Granulation in Magnetic versus Non-Magnetic
    Regions
Authors: Topka, K. P.; Tarbell, T. D.; SOUP Team
Bibcode: 1986BAAS...18..662T
Altcode:
  No abstract at ADS

Title: White-light movies of the solar photosphere from the soup
    instrument on spacelab 2
Authors: Title, A. M.; Tarbell, T. D.; Simon, G. W.; Acton, L.;
   Duncan, D.; Ferguson, S.; Finch, M.; Frank, Z.; Kelly, G.; Lindgren,
   R.; Morrill, M.; Pope, T.; Reeves, R.; Rehse, R.; Shine, R.; Topka,
   K.; Harvey, J.; Leibacher, J.; Livingston, W.; November, L.
Bibcode: 1986AdSpR...6h.253T
Altcode: 1986AdSpR...6..253T
  We present initial results on solar granulation, pores and sunspots
  from the white-light films obtained by the Solar Optical Universal
  Polarimeter (SOUP) instrument on Spacelab 2. SOUP contains a
  30-cm Cassegrain telescope, an active secondary mirror for image
  stabilization, and a white-light optical system with 35-mm film
  and video cameras. Outputs from the fine guidance servo provided
  engineering data on the performance of the ESA Instrument Pointing
  System (IPS). Several hours of movies were taken at various
  disk and limb positions in quiet and active regions. The images
  are diffraction-limited at 0.5 arc second resolution and are, of
  course, free of atmospheric seeing and distortion. Properties of the
  granulation in magnetic and non-magnetic regions are compared and are
  found to differ significantly in size, rate of intensity variation,
  and lifetime. In quiet sun on the order of fifty percent of the area
  has at least one ``exploding granule'' occurring in it during a 25
  minute period. Local correlation tracking has detected several types
  of transverse flows, including systematic outflow from the penumbral
  boundary of a spot, motion of penumbral filaments, and cellular flow
  patterns of supergranular and mesogranular size. Feature tracking has
  shown that in quiet sun the average granule fragment has a velocity
  of about one kilometer per second.

Title: Association of Small, Bright Photospheric Features with
    Magnetic Fields
Authors: Topka, K.; Shine, R.; SOUP Team
Bibcode: 1985BAAS...17..834T
Altcode:
  No abstract at ADS

Title: High Resolution Observations of Magnetic Features on the Sun
Authors: Topka, K. P.; Tarbell, T. D.
Bibcode: 1984BAAS...16..991T
Altcode:
  No abstract at ADS

Title: High Spatial Resolution Magnetic Observation of an Active
    Region
Authors: Topka, K.; Tarbell, T.
Bibcode: 1984ssdp.conf..278T
Altcode:
  High spatial resolution magnetograms of an active region reveal
  apparent changes in the magnetic flux of small isolated features on
  time scales less than 30 minutes. Both flux increases and decreases
  are observed, sometimes for a single feature. These changes are seen
  in small unipolar magnetic regions with no obvious changes observed
  in any nearby opposite polarity features.

Title: The Coordinated Instrument Package for the Solar Optical
    Telescope
Authors: Wolfson, C. J.; Tarbell, T. D.; Topka, K. P.; Title, A. M.
Bibcode: 1983BAAS...15R.718W
Altcode:
  No abstract at ADS

Title: Scientific Observing Plans for the SOT Coordinated Filtergraph
    Spectrograph
Authors: Tarbell, T. D.; Wolfson, C. J.; Topka, K. P.
Bibcode: 1983BAAS...15R.709T
Altcode:
  No abstract at ADS

Title: The SOT Video Data System
Authors: Topka, K. P.; Lindgren, R. W.; Duncan, D. W.
Bibcode: 1983BAAS...15Q.709T
Altcode:
  No abstract at ADS

Title: On the Disappearance of a Small Sunspot Group
Authors: Wallenhorst, S. G.; Topka, K. P.
Bibcode: 1982SoPh...81...33W
Altcode:
  The small sunspot group associated with Hale active region 17694
  was observed jointly by the Mount Wilson and the Big Bear Solar
  Observatories, through the time of sunspot disappearance. The magnetic
  flux from the region was seen to decrease by about 10% per day during
  the observing interval. This was accompanied by fragmentation of
  the dominant spot as a supergranule network formed. No evidence for
  spreading or diffusion of the active region field was found.

Title: Evidence for a Poleward Meridional Flow on the Sun
Authors: Topka, K.; Moore, R.; Labonte, B. J.; Howard, R.
Bibcode: 1982SoPh...79..231T
Altcode:
  We define for observational study two subsets of all polar zone
  filaments, which we call polemost filaments and polar filament
  bands. The behavior of the mean latitude of both the polemost filaments
  and the polar filament bands is examined and compared with the evolution
  of the polar magnetic field over an activity cycle as recently distilled
  by Howard and LaBonte (1981) from the past 13 years of Mt. Wilson
  full-disk magnetograms. The magnetic data reveal that the polar
  magnetic fields are built up and maintained by the episodic arrival of
  discrete f-polarity regions that originate in active region latitudes
  and subsequently drift to the poles. After leaving the active-region
  latitudes, these unipolar f-polarity regions do not spread equatorward
  even though there is less net flux equatorward; this indicates that
  the f-polarity regions are carried poleward by a meridional flow,
  rather than by diffusion. The polar zone filaments are an independent
  tracer which confirms both the episodic polar field formation and the
  meridional flow. We find: The mean latitude of the polemost filaments
  tracks the boundary of the polar field cap and undergoes an equatorward
  dip during each arrival of additional polar field.

Title: A magnitude limited stellar X-ray survey and the F star X-ray
    luminosity function.
Authors: Topka, K.; Golub, L.; Gorenstein, P.; Harnden, F. R., Jr.;
   Vaiana, G. S.; Avni, Y.; Rosner, R.
Bibcode: 1982ApJ...259..677T
Altcode:
  An X-ray survey has been conducted of stars brighter than visual
  magnitude 8.5 that have serendipitously fallen into the fields of view
  of the Imaging Proportional Counter of the Einstein Observatory. The
  survey includes 227 separate 1 x 1 deg fields, containing 274 stars
  with a visual magnitude of no more than 8.5 and covering a wide range
  of spectral types and luminosity classes. X-ray emission was detected
  from 33 stars, and upper limits have been determined for the remainder
  of the sample. F type stars dominate the detected sample, and most of
  these are shown to be dwarfs. An X-ray luminosity function for dF stars
  has been deduced, and reveals that the average 0.2-4.0 keV luminosity
  of these stars is around 10 to the 29th erg/sec. Constraints have been
  placed on the high luminosity tails and medians of the X-ray luminosity
  functions for other types of stars.

Title: Detection of microwave emission from both components of the
    red dwarfbinary EQ Peg.
Authors: Topka, K.; Marsh, K. A.
Bibcode: 1982ApJ...254..641T
Altcode:
  The detection at 4.9 GHz of the late main sequence binary EQ Pegasi
  (dM3.5e + dM4.5e) with the VLA is reported. Both components were
  detected, as flux levels of 0.69 mJy and 0.4 mJy, respectively. Thermal
  gyroresonance emission from the quiescent coronae of these stars appears
  to explain observations of the authors, as it does those of Gary and
  Linsky (1981) for chi Ori and UV Ceti, provided coronal magnetic fields
  in excess of 300 gauss exist over a region that has a length scale of
  at least twice the radii of these stars. Support for this model is
  provided by the unlikelihood of both stars flaring simultaneously,
  and by the fact that the emission was confined to each star within
  the observational uncertainty of a few AU.

Title: Death of a Sunspot
Authors: Topka, K. P.; Wallenhorst, S. G.
Bibcode: 1982BAAS...14..640T
Altcode:
  No abstract at ADS

Title: The stellar contribution to the galactic soft X-ray background
Authors: Rosner, R.; Avni, Y.; Bookbinder, J.; Giacconi, R.; Golub,
   L.; Harnden, F. R., Jr.; Maxson, C. W.; Topka, K.; Vaiana, G. S.
Bibcode: 1981ApJ...249L...5R
Altcode:
  Log N-log S relations for stars are constructed based on median
  X-ray luminosities for dF, dG, and dK stars previously reported for
  the Einstein Observatory/Center for Astrophysics stellar survey and
  on a detailed X-ray luminosity function derived here for dM stars,
  and the stellar contribution to the diffuse soft X-ray background is
  investigated. The principal results are that stars provide approximately
  20% of the soft X-ray background in the 0.28-1.0 keV passband and
  therefore contribute significantly to the soft X-ray background in this
  energy range (with dM stars constituting the dominant contributing
  class), and that the stellar contribution to the diffuse X-ray
  background in the 0.15-0.28 keV passband is less than approximately 3%.

Title: Results from an extensive Einstein stellar survey.
Authors: Vaiana, G. S.; Cassinelli, J. P.; Fabbiano, G.; Giacconi,
   R.; Golub, L.; Gorenstein, P.; Haisch, B. M.; Harnden, F. R., Jr.;
   Johnson, H. M.; Linsky, J. L.; Maxson, C. W.; Mewe, R.; Rosner, R.;
   Seward, F.; Topka, K.; Zwaan, C.
Bibcode: 1981ApJ...245..163V
Altcode:
  The preliminary results of the Einstein Observatory stellar X-ray survey
  are presented. To date, 143 soft X-ray sources have been identified with
  stellar counterparts, leaving no doubt that stars in general constitute
  a pervasive class of low-luminosity galactic X-ray sources. Stars along
  the entire main sequence, of all luminosity classes, pre-main sequence
  stars as well as very evolved stars have been detected. Early type
  OB stars have X-ray luminosities in the range 10 to the 31st to 10 to
  the 34th ergs/s; late type stars show a somewhat lower range of X-ray
  emission levels, from 10 to the 26th to 10 to the 31st ergs/s. Late type
  main-sequence stars show little dependence of X-ray emission levels upon
  stellar effective temperature; similarly, the observations suggest weak,
  if any, dependence of X-ray luminosity upon effective gravity. Instead,
  the data show a broad range of emission levels (about three orders of
  magnitude) throughout the main sequence later than F0.

Title: Absolute Light Curves of Solar Flares in Hα
Authors: Topka, K.; Hurford, G. J.
Bibcode: 1981BAAS...13..890T
Altcode:
  No abstract at ADS

Title: The Magnetic Evolution of Active Regions: Disappearance of
    Photospheric Magnetic Flux
Authors: Topka, K.; Moore, R. L.
Bibcode: 1980BAAS...12..792T
Altcode:
  No abstract at ADS

Title: Polar Crown Filaments and the Polar Magnetic Field
Authors: Topka, K.; Moore, R. L.; Labonte, B. J.; Howard, R.
Bibcode: 1980BAAS...12..893T
Altcode:
  No abstract at ADS

Title: X-Ray Observations of Stellar Coronae.
Authors: Topka, K. P.
Bibcode: 1980PhDT.........6T
Altcode:
  The Einstein X-Ray Observatory (HEAO-2) has been used to search for
  X-ray emission from a wide variety of stars in our galaxy. A significant
  fraction of the data was obtained via the 8.5 magnitude stellar survey,
  which is reported here. This survey searches for X-ray emission from
  all stars brighter than visual magnitude 8.5 that serendipitously fell
  into the Imaging Proportional Counter field-of-view of the Einstein
  Observatory. The survey includes 227 separate fields that contain a
  total of 276 stars with V &lt; 8.5. A wide range of spectral types and
  luminosity classes are represented. X-Ray emission in excess of 3-sigma
  above local background was discovered from 33 stars; 3-sigma upper
  limits have been determined for the remaining 243 stars. Comparison of
  X-ray source detection statistics with the expected frequency of stars
  brighter than V = 8.5 as a function of spectral type and luminosity
  class shows that the present visual magnitude limited survey can
  define the X-ray luminosity function for dwarf F stars and provides
  constraints for the high luminosity tails of the X-ray luminosity
  functions for other types of stars constructed from other Einstein
  observations. A second survey reported here is called the Gliese
  survey. This survey consists of all nearby stars listed in either of
  2 catalogues of the nearest stars that accidentally fell into any CFA
  (Center for Astrophysics) Einstein observation. A total of 29 nearby
  stars are included in the Gliese survey. Ten were detected, including 4
  dwarf M stars and 3 dwarf K stars. Late dwarf K and dwarf M stars are
  not effectively sampled by the 8.5 survey because most are fainter
  than 8.5 magnitude. The results of the 8.5 and Gliese survey have
  been integrated with those of four other Einstein surveys. In total,
  X-ray emission has been detected from 156 stars, with most of these
  representing initial discoveries. A correlation of X-ray luminosity
  with spectral type (soft X-ray H-R Diagram) is presented. Most of
  the observations can be explained by the presence of hot coronae
  around stars of nearly every spectral type. However, the data is at
  variance in many respects to existing theoretical coronal models based
  on acoustic flux dissipation. The consequences of these observations
  in terms of the presence of stellar outer convection zones, surface
  magnetic fields, and rotation rates are discussed.

Title: X-ray observations of stellar coronae
Authors: Topka, Kenneth P.
Bibcode: 1980PhDT.......105T
Altcode:
  No abstract at ADS

Title: Discovery of an X-ray star association in VI Cygni (Cyg OB2).
Authors: Harnden, F. R., Jr.; Branduardi, G.; Elvis, M.; Gorenstein,
   P.; Grindlay, J.; Pye, J. P.; Rosner, R.; Topka, K.; Vaiana, G. S.
Bibcode: 1979ApJ...234L..51H
Altcode:
  A group of six X-ray sources located within 0.4 deg of Cygnus X-3 has
  been discovered with the Einstein Observatory. These sources have been
  positively identified and five of them correspond to stars in the
  heavily obscured OB association VI Cygni. The optical counterparts
  include four of the most luminous O stars within the field of view
  and a B5 supergiant. These sources are found to have typical X-ray
  luminosities of 5 x 10 to the 33rd ergs/s, with temperatures of 10 to
  the 6.8th K and hydrogen column densities of 10 to the 22nd/sq cm,
  and therefore comprise a new class of low-luminosity galactic X-ray
  sources associated with early-type stars.

Title: X-ray Observations of the α Cen System from EINSTEIN.
Authors: Golub, L.; Harnden, F. R., Jr.; Rosner, R.; Topka, K.;
   Vaiana, G. S.
Bibcode: 1979BAAS...11..775G
Altcode:
  No abstract at ADS

Title: X-ray Observations of Very Late-Type Dwarf Stars from the
    EINSTEIN Observatory.
Authors: Rosner, R.; Giacconi, R.; Golub, L.; Harnden, F. R., Jr.;
   Topka, K.; Vaiana, G. S.
Bibcode: 1979BAAS...11..776R
Altcode:
  No abstract at ADS

Title: On Stars and OB Associations Observed from EINSTEIN.
Authors: Harnden, F. R., Jr.; Golub, L.; Rosner, R.; Seward, F.;
   Topka, K.; Vaiana, G. S.
Bibcode: 1979BAAS...11..775H
Altcode:
  No abstract at ADS

Title: A Magnitude Limited Stellar Survey with EINSTEIN.
Authors: Topka, K.; Golub, L.; Harnden, F. R., Jr.; Gorenstein, P.;
   Rosner, R.; Vaiana, G. S.
Bibcode: 1979BAAS...11..781T
Altcode:
  No abstract at ADS

Title: The Einstein (HEAO 2) X-ray Observatory.
Authors: Giacconi, R.; Branduardi, G.; Briel, U.; Epstein, A.;
   Fabricant, D.; Feigelson, E.; Forman, W.; Gorenstein, P.; Grindlay,
   J.; Gursky, H.; Harnden, F. R.; Henry, J. P.; Jones, C.; Kellogg,
   E.; Koch, D.; Murray, S.; Schreier, E.; Seward, F.; Tananbaum, H.;
   Topka, K.; Van Speybroeck, L.; Holt, S. S.; Becker, R. H.; Boldt,
   E. A.; Serlemitsos, P. J.; Clark, G.; Canizares, C.; Markert, T.;
   Novick, R.; Helfand, D.; Long, K.
Bibcode: 1979ApJ...230..540G
Altcode:
  The Einstein (HEAO 2) X-ray Observatory, launched in 1978, includes
  a fully imaging focusing X-ray telescope with an angular resolution
  of a few arc sec, a field of view of up to one deg, and a sensitivity
  several hundred times greater than previously available in any X-ray
  astronomy experiment. A high-resolution imager, an imaging proportional
  counter, a focal plane crystal spectrometer, and a monitor proportional
  counter are among the principal instruments on board the Einstein
  X-ray Observatory. About 20% of the total effective observing time
  in the first year of the X-ray astronomy experiment has been reserved
  for guest observers.

Title: Soft X-ray structure of the Coma cluster of galaxies.
Authors: Gorenstein, P.; Fabricant, D.; Topka, K.; Harnden, F. R., Jr.
Bibcode: 1979ApJ...230...26G
Altcode:
  Results are reported for an observation of the Coma cluster with
  an imaging X-ray telescope system aboard a sounding rocket. A
  two-dimensional X-ray map of the cluster in the energy range from
  0.15 to 2.0 keV is presented. The radial distribution, granularity,
  and ellipticity of the X-ray surface brightness are investigated, and
  the spectrum and flux within the field of view are analyzed. These
  properties are then examined quantitatively by comparing the
  observations with models through the use of a chi-squared test. It is
  found that: (1) no single galaxy contributes more than a few percent
  of the total X-ray flux of the Coma cluster; (2) the X-ray source
  is diffuse but granular on a scale of several arcmin, particularly
  in the central region; (3) the centroid of the X-ray source is at a
  local intensity minimum; and (4) the data are most consistent with an
  isothermal hydrostatic model.

Title: Detection of soft X-rays from alpha Lyrae and eta Bootis with
    an imaging X-ray telescope.
Authors: Topka, K.; Fabricant, D.; Harnden, F. R., Jr.; Gorenstein,
   P.; Rosner, R.
Bibcode: 1979ApJ...229..661T
Altcode:
  Results are presented for observations of Alpha Lyr (Vega) and Eta
  Boo with an imaging X-ray telescope during two rocket flights. It is
  found that Vega and Eta Boo are soft X-ray sources with respective
  luminosities of approximately 3 x 10 to the 28th erg/s (0.15-0.8 keV)
  and 1 x 10 to the 29th erg/s (0.15-1.5 keV). Surface X-ray luminosities
  of about 640,000 erg/sq cm per sec for Vega and 300,000 erg/sq cm
  per sec for Eta Boo are estimated and shown to fall within the range
  of solar coronal X-ray emission. It is concluded that in view of the
  substantially larger surface areas of these stars, the relatively large
  total soft X-ray luminosity (as compared with that of the sun) can in
  both cases be understood as resulting from a moderately active corona,
  although the Vega observation is in severe conflict with simple models
  for X-ray emission from single main-sequence stars.

Title: Initial Results from the Einstein Survey of Stellar
    Low-Luminosity X-ray Sources
Authors: Vaiana, G.; Forman, W.; Giacconi, R.; Gorenstein, P.; Pye,
   J.; Rosner, R.; Seward, F.; Topka, K.
Bibcode: 1979BAAS...11..446V
Altcode:
  No abstract at ADS

Title: Spatially resolved measurements of an Fe XVII-XXIV X-ray line
    complex in the halo of M87 with an imaging telescope.
Authors: Fabricant, D.; Topka, K.; Harnden, F. R., Jr.; Gorenstein, P.
Bibcode: 1978ApJ...226L.107F
Altcode:
  No abstract at ADS

Title: Soft X-ray structure of the Perseus cluster of galaxies.
Authors: Gorenstein, P.; Fabricant, D.; Topka, K.; Harnden, F. R.,
   Jr.; Tucker, W. H.
Bibcode: 1978ApJ...224..718G
Altcode:
  A 0.5-1.5-keV X-ray image of the Perseus cluster of galaxies was
  obtained with a focusing telescope system aboard a sounding rocket. The
  source consists of a region of diffuse emission plus a superposed
  central source in the vicinity of NGC 1275 smaller than 4 arcmin in
  diameter that accounts for one-quarter of the total intensity within a
  radius of 25 arcmin. The results for the diffuse source are consistent
  with the isothermal-hydrostatic picture in which the hot gas has a
  core radius of 17 arcmin and is approximately symmetric about NGC
  1275. Several isothermal-hydrostatic models are considered which
  relate the size and temperature of the diffuse X-ray source with the
  core radius of the galaxies and their velocity dispersion. Fixing the
  velocity dispersion at values measured by Chincarini and Rood (1971)
  requires the core radius of the galaxies to be 28 + or - 9 arcmin, which
  is larger than present measurements. Conversely, fixing the core radius
  of the galaxies at 8 arcmin requires a smaller velocity dispersion or
  a condition in which the velocity distribution is anisotropic. Upper
  limits on the intrinsic X-ray absorption of the central source place
  the bulk of its X-ray emission beyond the nuclear region of NGC 1275.

Title: Structure of the X-ray source in the Virgo cluster of galaxies.
Authors: Gorenstein, P.; Fabricant, D.; Topka, K.; Tucker, W.; Harnden,
   F. R., Jr.
Bibcode: 1977ApJ...216L..95G
Altcode:
  High-angular-resolution observations in the 0.15-1.5-keV band with an
  imaging X-ray telescope shows the extended X-ray source in the Virgo
  cluster of galaxies to be a diffuse halo of about 15 arcmin core radius
  surrounding M87. The angular structure of the surface brightness
  is marginally consistent with either of two simple models: (1) an
  isothermal (or adiabatic or hydrostatic) sphere plus a point source
  at M87 accounting for 12% of the total 0.5-1.5-keV intensity or (2)
  a power-law function without a discrete point source. No evidence for
  a point source is seen in the 0.15-0.28-keV band, which is consistent
  with self-absorption by about 10 to the 21st power per sq cm of matter
  having a cosmic abundance. The power-law models are motivated by the
  idea that radiation losses regulate the accretion of matter onto M87
  and can account for the observed difference in the size of the X-ray
  source as seen in the present measurements and at higher energies.

Title: Short Observations of Bright Stars with a Rocket Borne Imaging
    X-Ray Telescope.
Authors: Topka, K.; Fabricant, D.; Harnden, F. R., Jr.; Gorenstein, P.
Bibcode: 1977BAAS....9..560T
Altcode:
  No abstract at ADS

Title: Soft X-Ray Structure of the Coma Cluster of Galaxies
Authors: Gorenstein, P.; Fabricant, D.; Topka, K.; Harnden, F. R., Jr.
Bibcode: 1977BAAS....9..560G
Altcode:
  No abstract at ADS

Title: Comparison of X-Ray Structure of Clusters of Galaxies with
    Thermal Models of the Intracluster Gas.
Authors: Fabricant, D.; Topka, K.; Harnden, F. R., Jr.; Gorenstein, P.
Bibcode: 1977BAAS....9..560F
Altcode:
  No abstract at ADS

Title: A soft X-ray image of the Algol region.
Authors: Harnden, F. R., Jr.; Fabricant, D.; Topka, K.; Flannery,
   B. P.; Tucker, W. H.; Gorenstein, P.
Bibcode: 1977ApJ...214..418H
Altcode:
  Algol (Beta Persei) has been detected in two separate exposures of
  an imaging X-ray telescope. The 0.15- to 2-keV X-ray luminosity is
  approximately 2 by 10 to the 30th power erg/s. The X-ray flux is
  interpreted as thermal emission produced by direct accretion of mass
  from the K star to the B8 member of the triple star system.

Title: An X-Ray Image of M87 and the Virgo Cluster of Galaxies.
Authors: Gorenstein, P.; Topka, K.; Fabricant, D.; Harnden, F. R., Jr.
Bibcode: 1976BAAS....8..553G
Altcode:
  No abstract at ADS

Title: Detection of η Bootes with an Imaging X-Ray Telescope.
Authors: Harnden, F. R., Jr.; Fabricant, D.; Topka, K.; Gorenstein, P.
Bibcode: 1976BAAS....8..529H
Altcode:
  No abstract at ADS

