Author name code: rhodes
ADS astronomy entries on 2022-09-14
author:"Rhodes, Edward J. Jr." OR author:"Rhodes, E.J. Jr." -aff:"Sheffield" -aff:"Earth" -author:"Rhodes, Elizabeth"
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Title: Sub-surface Meridional Flow Results from MWO, GONG, and MDI
    during Solar Cycle 23
Authors: Pinkerton, Stephen; Rhodes, Edward J.; Bogart, Richard S.
Bibcode: 2014AAS...22421823P
Altcode:
  Time series of full-disk Dopplergrams were acquired at the 60-Foot
  Solar tower of the Mount Wilson Observatory every year between 1987
  and 2009. Analysis of this archive revealed that the focal plane of
  the Tower did experience a small amount of systematic rotation, which
  suggested that the alignment of the optics had changed slightly over
  the years since its construction in 1907. This has caused some of the
  initial daily flow maps to possess a so-called “washing machine”
  effect similar to the pattern that was seen in raw GONG flow maps. We
  have incorporated a systematic program of ring-diagram analysis in
  which we have tracked the raw solar images using five differing assumed
  instrumental rotation rates. We have then gone on to compute synoptic
  maps of the horizontal flow vectors at several different depths over
  much of Solar Cycle 23 in order to study how such an instrumental
  rotation might affect both the zonal and meridional flows as functions
  of latitude, depth, and time. We compare these results with GONG and MDI
  flow measurements to empirically determine the regime within which the
  MWO results are reliable and extend our analysis into Solar Cycle 22.

Title: Optically Stimulated Luminescence Dating of Sediments over
    the Past 200,000 Years
Authors: Rhodes, Edward J.
Bibcode: 2011AREPS..39..461R
Altcode:
  Optical dating of sediment using optically stimulated luminescence
  has become important for studying Earth surface processes, and this
  technique continues to develop rapidly. A group of closely linked
  luminescence methods can be used to estimate the time since grains of
  quartz and feldspar were last exposed to daylight by detecting their
  subsequent response to environmental ionizing radiation exposure. The
  technique is well suited to the dating of deposits as young as one year
  to several hundred thousand years. Recent technical developments have
  established a dating protocol with improved precision, a high degree
  of reliability, and an in-built means to detect incomplete signal
  removal during deposition. This approach has been extended to age
  estimation for single grains, opening up a wider range of potential
  environments and new possibilities for understanding postdepositional
  grain movement. Ongoing research offers the possibility of significant
  age range extension and novel applications including low-temperature
  thermochronology.

Title: Miniature Neutron-Alpha Activation Spectrometer
Authors: Rhodes, Edgar; Holloway, James Paul; He, Zhong; Goldsten, John
Bibcode: 2002AIPC..632..101R
Altcode:
  We are developing a miniature neutron-alpha activation spectrometer for
  in-situ analysis of chem-bio samples, including rocks, fines, ices,
  and drill cores, suitable for a lander or Rover platform for Mars or
  outer-planet missions. In the neutron-activation mode, penetrating
  analysis will be performed of the whole sample using a γ spectrometer
  and in the α-activation mode, the sample surface will be analyzed
  using Rutherford-backscatter and x-ray spectrometers. Novel in our
  approach is the development of a switchable radioactive neutron source
  and a small high-resolution γ detector. The detectors and electronics
  will benefit from remote unattended operation capabilities resulting
  from our NEAR XGRS heritage and recent development of a Ge γ detector
  for MESSENGER. Much of the technology used in this instrument can be
  adapted to portable or unattended terrestrial applications for detection
  of explosives, chemical toxins, nuclear weapons, and contraband.

Title: Observed and Predicted Ratios of the Horizontal and Vertical
    Components of the Solar p-Mode Velocity Eigenfunctions
Authors: Rhodes, Edward J., Jr.; Reiter, Johann; Schou, Jesper;
   Kosovichev, Alexander G.; Scherrer, Philip H.
Bibcode: 2001ApJ...561.1127R
Altcode:
  We present evidence that the observed ratios of the horizontal
  and vertical components of the solar intermediate-degree p-mode
  velocity eigenfunctions closely match theoretical predictions of
  these ratios. This evidence comes from estimates of the observed
  eigenfunction component ratios that were obtained from the fitting
  of the p-mode oscillation peaks in low- and intermediate-degree
  (l&lt;=200) m-averaged power spectra computed from two different
  60.75 day time series of Global Oscillation Network Group (GONG)
  project Dopplergrams obtained in late 1996 and early 1998. These fits
  were carried out using a peak-fitting method in which we fitted each
  observed p-mode multiplet with a model profile that included both the
  target mode and its six nearest spatial sidelobes and which incorporated
  the effects of the incomplete observational time series through the
  convolution of the fitted profiles with the temporal window functions,
  which were computed using the two actual GONG observing histories. The
  fitted profile also included the effects of the spatial leakage of
  the modes of differing degrees into the target spectrum through the
  use of different sets of m-averaged spatial leakage matrices. In
  order to study the sensitivity of the estimated component ratios to
  the details of the computation of the m-averaged power spectra and of
  the image-masking schemes employed by the GONG project, we generated
  a total of 22 different sets of modal fits. We found that the best
  agreement between the predicted and inferred ratios came from the use
  of unweighted averaged power spectra that were computed using so-called
  n-averaged frequency-splitting coefficients, which had been computed
  by cross-correlating the 2l+1 zonal, tesseral, and sectoral power
  spectra at each l over a wide range of frequencies. This comparison
  yielded a total of 1906 pairs of predicted c<SUB>t,theory</SUB> and
  fitted c<SUB>t,fit</SUB> eigenfunction component ratios. A linear
  regression analysis of these pairs of ratios resulted in the following
  regression equation: c<SUB>t,fit</SUB>=(0.0088+/-0.0013)+(0.9940+/-
  0.0044)c<SUB>t,theory</SUB>. The resulting correlation coefficient
  was 0.9817. This agreement between the predicted and inferred ratios
  suggests that the predicted ratios should be used in the fitting of
  high-degree power spectra where the ratios cannot be inferred because
  of the blending together of individual modal peaks into broad ridges
  of power.

Title: Helioseismology: A probe of the solar interior, atmosphere,
    and activity cycle
Authors: Rhodes, Edward J.
Bibcode: 1996AIPC..382....3R
Altcode:
  Helioseismology began in earnest in the mid-1970s. By 1977
  helioseismology had demonstrated that the solar convection zone was
  about twice as deep as was previously thought to be the case. Since then
  helioseismology has also provided a measurement of the radial profile
  of the sound speed in the solar interior and it has also ruled out
  solar models which would attempt to solve the solar neutrino problem
  through a lowering of the temperature of the core, while at the same
  time showing that the effects of the diffusion of helium and other
  elements must be incorporated in the computation of the most accurate
  models of the solar interior. The field has also provided measurements
  of the radial and latitudinal profiles of the sun's angular velocity
  over the outer half of the solar interior (as measured by radius). It
  has also provided evidence for helical flow patterns in the motions of
  the very shallow, sub-photospheric layers. Finally, the frequencies
  of the solar p-mode oscillations have also been demonstrated to vary
  with changing levels of solar activity.

Title: Confirmation of Solar Cycle--dependent Intermediate-Degree
    p-Mode Frequency Shifts
Authors: Rhodes, Edward J., Jr.; Cacciani, Alessandro; Korzennik,
   Sylvain G.; Ulrich, Roger K.
Bibcode: 1993ApJ...406..714R
Altcode:
  Results of intercomparisons of seven different sets of frequencies of
  intermediate-degree p-modes obtained at several different locations
  between 1981 and 1989 are presented. It is shown that the frequency
  shifts exhibited by all of these intermediate-degree p-modes are
  consistent with the intermediate-degree frequency shifts presented by
  Libbrecht and Woodward (1990) and also with the low-degree frequency
  shifts presented by Elsworth et al. (1990). It is also shown that these
  frequency shifts correlate with solar cycle-dependent changes in sunspot
  number, area, and irradiance. Unbinned and binned differences between
  1984 Mount Wilson Observatory and revised 1981 South Pole frequencies
  are illustrated.

Title: The Supergranulation Spectrum
Authors: Hathaway, David H.; Rhodes, Edward J.; Cacciani, Alessandro;
   Korzennik, Sylvain G.
Bibcode: 1991LNP...388..163H
Altcode: 1991ctsm.conf..163H
  Full-disk Dopplergram observations obtained at the 60-foot
  tower of the Mount Wilson Observatory with the Cacciani sodium
  magneto-optical filter were analyzed to determine the spectrum of
  the solar supergranulation. Individual Dopplergrams were averaged
  together using a weighted average over 20-minute intervals to remove
  the p-mode oscillations. The Doppler signals due to the motion of the
  observer, the solar rotation, differential rotation, and limb shift
  were then removed from the data to produce Dopplergrams dominated
  by the supergranular flows. These data were mapped to heliographic
  coordinates and projected onto the spherical harmonics. The resulting
  spectrum exhibits a peak at spherical harmonic degree } 100, which
  corresponds to typical cell diameters of about 40 Mm. Synthetic data
  were constructed and passed through the same analysis procedures to
  determine the actual spectrum required to reproduce the results. A
  good fit was obtained with a kinetic energy spectrum which peaks at }
  100 and decreases exponentially out to } 500 with an e-folding range
  of } 90. A power law fit to the spectrum over this range in yields an
  exponent of about -2.75. No corrections for seeing were included in
  the analysis. Although the image was sampled at 8 arcsec resolution,
  the effects of seeing may alter the actual slope of the spectrum and
  make it somewhat flatter. The spectrum does not exhibit any evidence
  for a distinct mesogranulation component out to } 500 (corresponding
  to cell diameters of about 8 Mm).

Title: Solar Oscillation Ring Diagrams from Mt. Wilson Full-Disk
    Magneto-Optical Dopplergrams
Authors: Hill, Frank; Rhodes, Edward J.; Korzennik, Sylvain G.;
   Cacciani, Alessandro; Brown, Timothy M.
Bibcode: 1991LNP...388..271H
Altcode: 1991ctsm.conf..271H
  Three-dimensional power spectra of solar oscillations have been
  computed from moderate-resolution full disk Doppler images obtained
  with the Magneto-Optical Filter at Mt. Wilson. Slices of the spectra
  at constant frequency reveal the ring structures that are analogous
  to the ridges in two-dimensional spectra. Ring diagrams obtained
  at different heliographic positions show large differences in the
  structure of the rings. These variations can be attributed to the
  changing effective spatial resolution of the observations across the
  disk. After correction for this effect, and .for terrestrial seeing,
  the rings will be used to map the horizontal flows in the convection
  zone as a function of position and depth.

Title: Measurements of Intermediate- and High-Degree (20&lt;1&lt;600)
    p-Mode Solar Oscillation Power and Energy
Authors: Rhodes, Edward J.; Brown, Timothy M.; Cacciani, Alessandro;
   Korzennik, Sylvain G.; Ulrich, Roger K.
Bibcode: 1991LNP...388..277R
Altcode: 1991ctsm.conf..277R
  We present measurements of the total modal power and energy of
  both intermediate- and high-degree (20&lt; l &lt;600) solar p-mode
  oscillations which have been corrected to first order for the combined
  effects of atmospheric seeing, image motion due to imperfect tracking,
  and the point spread function of our optics. These power and energy
  estimates have been obtained from an average of 20 separate zonal l -
  n power spectra, which were obtained from observations obtained at the
  60-Foot Solar Tower of the Mt. Wilson Observatory between July 1 and 20,
  1988. The raw total power values were obtained from a least-squares
  fitting of Lorentzian profiles to the p-mode ridges in the average
  zonal power spectrum. As an initial method of correcting the observed
  power levels, we adopted the procedure described by Kaufman (1988)
  and deconvolved measurements of the observed limb profiles from one
  of our images using two slightly different theoretical unblurred limb
  profiles in order to obtain two estimates of the modulation transfer
  function (mtf) of our experiment. The corrected power values which
  resulted show systematic variations with both frequency and degree
  which are similar to those obtained by Kaufman. For example, between
  l = 100 and 600 our corrected power values drop by a factor of at
  least 4.5, although the magnitude of our correction becomes less
  certain as the degree is increased above 300. We also convert these
  power values into estimates of the total energy of the modes to show
  that the modal energies decrease by a factor of at least 15 over the
  same range in l. Even given the uncertainty of our correction at the
  higher degrees, the consistency of the l-dependent decrease in the
  modal energies with similar results by Kaufman (1990) suggests that,
  at least above l = 100, the modes are not in energy equipartition with
  turbulent convective eddies.

Title: Further Evidence for Radial Variations in the Solar Equatorial
    Angular Velocity Profile
Authors: Rhodes, Edward J.; Cacciani, Alessandro; Korzennik, Sylvain
   G.; Ulrich, Roger K.
Bibcode: 1991LNP...388..285R
Altcode: 1991ctsm.conf..285R
  One year ago we presented evidence that the rotationally-induced
  frequency splittings of intermediate- and high-degree sectoral p-mode
  oscillations vary systematically as a function of the degree, l,
  of the modes (Rhodes, Cacciani, and Korzennik, 1989. Recently, we
  confirmed the results presented there in three different ways. First,
  we extended our earlier 5-day sequence of Dopplergrams to one of 20 days
  which ran from July 1 through 20, 1988. We then repeated our earlier
  cross-correlation analysis using the intrinsically higher frequency
  resolution sectoral power spectra which resulted from the longer
  data string. This analysis also showed the same l-dependence of the
  frequency splittings which we had found in our earlier work. Second,
  we computed a separate pair of 1024-minute long sectoral power
  spectra for each of the 20 days and then averaged the 20 prograde
  and 20 retrograde spectra into two average sectoral spectra. We
  next computed the frequencies of the centers of both the prograde
  and retrograde sectoral ridges at each even-l by fitting Lorentzian
  profiles using a standard non-linear least-squares method and we then
  simply subtracted the central frequencies of the corresponding prograde
  and retrograde ridges at those same values of l. The splittings which
  resulted from averaging these frequency differences over both l and
  the radial overtone, n, showed the same l-dependence as did those
  obtained from the cross-correlation analysis. Thirdly, we computed
  Legendre coefficient expansions to the m - v frequency shifts of both
  the high- and low-resolution tesseral power spectra. We then normalized
  the sums of the odd Legendre expansion coefficients to obtain additional
  estimates of the sectoral frequency splittings. Finally, we carried out
  an inversion of the sectoral frequency splittings. This inversion shows
  a rapid rise in the solar equatorial angular velocity from its surface
  value to a value of 476 nHz at a depth of 0.07 to 0.08 solar radii below
  the photosphere. The inverted profile also shows that the inner half
  of the solar convection zone may be rotating at the magnetic feature
  rate and that the equatorial angular velocity decreases inwardly of
  the base of the convection zone to a depth of at least 0.50 solar radii.

Title: Summary of the Institute of Theoretical Physics (ITP) program
    on helioseismology (Santa Barbara, January-June 1990)
Authors: Däppen, Werner; Rhodes, Ed
Bibcode: 1991AdSpR..11d..15D
Altcode: 1991AdSpR..11...15D
  The authors presented their view as participants of the ITP programme
  on helioseismology, which was coordinated by D.O. Gough and J. Toomre
  (Santa Barbara, Jan 1990 - June 1990). Detailed proceedings can be found
  in ``Challenges to theories of the structure of moderate-mass stars''
  (eds. D.O. Gough and J. Toomre, Springer, Heidelberg, 1991).

Title: Depth and Latitude Dependence of the Solar Internal Angular
    Velocity
Authors: Rhodes, Edward J., Jr.; Cacciani, Alessandro; Korzennik,
   Sylvain; Tomczyk, Steven; Ulrich, Roger K.; Woodard, Martin F.
Bibcode: 1990ApJ...351..687R
Altcode:
  One of the design goals for the dedicated helioseismology observing
  state located at Mount Wilson Observatory was the measurement of the
  internal solar rotation using solar p-mode oscillations. In this paper,
  the first p-mode splittings obtained from Mount Wilson are reported
  and compared with those from several previously published studies. It
  is demonstrated that the present splittings agree quite well with
  composite frequency splittings obtained from the comparisons. The
  splittings suggest that the angular velocity in the solar equatorial
  plane is a function of depth below the photosphere. The latitudinal
  differential rotation pattern visible at the surface appears to persist
  at least throughout the solar convection zone.

Title: Contribution of High-Degree Frequency Splittings to the
    Inversions of the Solar Rotation Rate
Authors: Korzennik, Sylvain G.; Cacciani, Alessandro; Rhodes, Edward
   J.; Ulrich, Roger K.
Bibcode: 1990LNP...367..341K
Altcode: 1990psss.conf..341K
  We present the contribution of high degree rotational splittings to
  the inversion of the internal rotation rate around the equator. The
  extention of the input data set to l of 500, allow us to improve the
  resolution of the solution mainly in the outermost 15% of the solar
  radius. The rotational profile obtained in the regions below the
  surface leads to an attractive picture that could reconcile different
  non-seismic estimates of the surface rotation rate.

Title: Evidence for Radial Variations in the Equatorial Profile of
    the Solar Internal Angular Velocity
Authors: Rhodes, Edward J.; Cacciani, Alessandro; Korzennik, Sylvain G.
Bibcode: 1990LNP...367..163R
Altcode: 1990psss.conf..163R
  We present evidence that the solar internal angular velocity, at least
  as measured in the equatorial plane, shows systematic radial variations
  in the outer half (by radius of the solar interior. Specifically,
  we employ the rotationally-induced frequency splittings of both high-
  and intermediate-degree sectoral p-mode oscillations to demonstrate
  that the internal angular velocity rises inwardly from the observed
  spectroscopic rotation rate of the photospheric gas to a higher value
  that is at least equal to the observed rotation rate of sunspots, if
  not higher, in the outer third of the convection zone before decreasing
  inward of the convection zone to a value which is at least two percent
  below the photospheric gas rotation rate. By making the assumption that
  the observed splittings are sensitive to solar rotation at the midpoints
  of the p-mode eigenfunctions we obtain an angular velocity profile which
  rises from 452 nHz at the photosphere to 462 nHz at a depth of about
  five percent of the solar radius below the photosphere. A comparison of
  this inferred angular velocity profile with that obtained from a formal
  inversion of these splittings (which is reported elsewhere in these
  proceedings by Korzennik et al.) suggests that the angular velocity
  might actually exceed the magnetic rotation rate over much of the
  convection zone before decreasing inwardly toward the center of the sun.

Title: Measurement of the rotational frequency splitting of the solar
    five-minute oscillations from magneto-optical filter observations.
Authors: Tomczyk, Steven; Cacciani, Alessandro; Korzennik, Sylvain G.;
   Rhodes, Edward J., Jr.; Ulrich, Roger K.
Bibcode: 1988ESASP.286..141T
Altcode: 1988ssls.rept..141T
  Observations of the solar five-minute oscillations in the photospheric
  velocity field were obtained during the summer of 1984 at the 60-foot
  solar tower of the Mt. Wilson Observatory with a magneto-optical
  filter. The magneto-optical filter employs magneto-optical effects in
  an atomic vapor to isolate narrow bandpasses in alternate wings of
  a spectral line. Time series of full disk velocity images having a
  resolution of about 10 arcseconds and a noise level of 15 m/s/pixel
  were obtained on 92 days between the months of May and September of
  1984. A subset of two time series from this data of 16 and 19 days
  duration having a total of 25744 doppler images were analyzed to provide
  estimates of the rotational frequency splitting for spherical harmonic
  degrees between 5 and 120. The results of this analysis indicate a
  decrease in the rate of solar rotation with increasing depth inside
  the sun. Also, a decrease in the rate of differential rotation with
  increasing depth is observed.

Title: Inversion of the solar rotation rate versus depth and latitude.
Authors: Korzennik, Sylvain G.; Cacciani, Alessandro; Rhodes, Edward
   J., Jr.; Tomczyk, Steven; Ulrich, Roger K.
Bibcode: 1988ESASP.286..117K
Altcode: 1988ssls.rept..117K
  The authors have used three different inversion techniques to compute
  the internal solar rotation rate from several sets of n-averaged
  frequency splittings. They have used an iterative variation of the
  spectral expansion method, the optimal averaging kernel method and
  a piecewise constant constrained least square method to invert the
  data. Each computation was carried out independently. While they
  present similar trends, each of the solutions differs in detail. A
  consistent feature in all the inversions is the disappearance of
  differential rotation below the base of the convection zone. Also,
  a strong differential signature in the deeper part of the convection
  zone is present in most of the solutions. A slow decrease of the
  rotation rate with depth for the equatorial and mid-latitude curves
  is significant in the spectral expansion and the least square results
  but only marginally apparent in the averaging kernel results.

Title: Acquisition and reduction procedures for MOF
    Doppler-magnetograms.
Authors: Cacciani, Alessandro; Ricci, D.; Rosati, P.; Rhodes, Edward
   J., Jr.; Smith, E.; Tomczyk, Steven; Ulrich, Roger K.
Bibcode: 1988ESASP.286..185C
Altcode: 1988ssls.rept..185C
  The authors analyse defects occurred on the MOF first magnetograms,
  particularly they discuss the problem of the apparent contamination
  between velocity and magnetic fields. They find that a correct
  acquisition and reduction procedure gives cleaner results. The authors
  also suggest a new vector magnetograph and compute the vector field
  at coronal levels using one MOF longitudinal magnetogram.

Title: Radial and latitudinal gradients in the solar internal
    angular velocity.
Authors: Rhodes, Edward J., Jr.; Cacciani, Alessandro; Korzennik,
   Sylvain G.; Tomczyk, Steven; Ulrich, Roger K.; Woodard, Martin F.
Bibcode: 1988ESASP.286...73R
Altcode: 1988ssls.rept...73R
  The authors recently presented the results of an analysis of the
  frequency splittings of intermediate-degree (3 &lt; degree ≤ 170)
  p-mode oscillations which were obtained from a 16-day subset of our 1984
  Mt. Wilson 60-foot tower observations. These results showed evidence
  for both radial and latitudinal gradients in the solar internal
  angular velocity. In particular, the results indicated that, from
  0.6 R<SUB><SUB>sun</SUB></SUB> to 0.95 R<SUB><SUB>sun</SUB></SUB>,
  the solar internal angular velocity increases systematically from
  440 to 463 nHz, corresponding to a positive radial gradient of ≍66
  nHz/R<SUB><SUB>sun</SUB></SUB> for that portion of the solar interior. A
  previous analysis indicated that the latitudinal differential rotation
  gradient which is seen at the solar surface persists throughout
  the convection zone, although there was some indication that the
  differential rotation might disappear entirely below the base of the
  convection zone. Here the authors extend their previous analysis to
  include comparisons with additional observational studies and they
  also present comparisons between our earlier results and the results
  of additional inversions of several of the observational datasets. All
  of these comparisons reinforce the previous conclusions regarding
  the existence of radial and latitudinal gradients in the internal
  angular velocity.

Title: Initial high-degree p-mode frequency splittings from the 1988
    Mt. Wilson 60-foot tower solar oscillation program.
Authors: Rhodes, Edward J., Jr.; Cacciani, Alessandro; Korzennik,
   Sylvain G.
Bibcode: 1988ESASP.286...81R
Altcode: 1988ssls.rept...81R
  The authors present here the initial frequency splitting results
  of solar p-mode oscillations which they have obtained from their
  1988 helioseismology at the Mt. Wilson Observatory. These frequency
  splittings correspond to the rotational splittings of sectoral harmonics
  which range in degree between 10 and 598. They were obtained from a
  cross-correlation analysis of the prograde and retrograde portions
  of a two-dimensional (l-ν) power spectrum. This power spectrum was
  computed from an eight-hour sequence of full-disk Dopplergrams which
  were obtained on July 2, 1988, at the 60-foot tower telescope with
  a Na magneto-optical filter and a 1024×1024 pixel CCD camera. These
  frequency splittings have an inherently larger scatter than did the
  splittings obtained from earlier 16-day power spectra. Consequently,
  the best one can say now is that these splittings are consistent with an
  internal solar rotational velocity which is independent of radius along
  the equatorial plane. The normalized frequency splittings averaged
  449±3 nHz, a value which is very close to the observed equatorial
  rotation rate of the photospheric gas of 451.7 nHz.

Title: Full-disk magnetograms obtained with a NA magneto-optical
    filter at the Mount Wilson Observatory
Authors: Rhodes, Edward J., Jr.; Cacciani, Alessandro; Garneau, Glenn;
   Misch, Tony; Progovac, Dusan; Shieber, Tom; Tomczyk, Steve; Ulrich,
   Roger K.
Bibcode: 1988fnsm.work...33R
Altcode:
  The first full-disk magnetograms to be obtained with the Na
  magneto-optical filter (MOF) which is located at the 60 foot solar
  tower of the Mount Wilson Observatory are presented. This MOF was
  employed as a longitudinal magnetograph on June 18, 19, and July 1,
  1987. On those three days the MOF was combined with a large format
  (1024 x 1024 pixel) virtual phase change coupled device camera and
  a high-speed data acquisition system. The combined system was used
  to record both line-of-sight magnetograms and Dopplergrams which
  covered the entire visible solar hemisphere. The pixel size of these
  magnetograms and Dopplergrams was 2.3 arcseconds. On each of the three
  days a time series of nine pairs of magnetograms and Dopplergrams
  was obtained at the rate of one pair every two minutes. On the same
  three day longitudinal magnetograms have one arcsecond pixels were
  obtained with the vacuum telescope at Kitt Peak. The MOF and vacuum
  tower magnetograms were compared at both the JPL Multi-Mission Image
  Processing Laboratory and at USC and have found the two sets of images
  to be well correlated both in spatial distribution and strength of the
  measured magnetic field. The simultaneously-obtained MOF Dopplergrams to
  remove the crosstalk which was present between the Doppler and Zeeman
  shifts of the NaD lines from the magnetograms from all three days and
  will also describe recent improvements to the system which allowed the
  obtaining of full-disk magnetograms as rapidly as one every 25 seconds.

Title: On the Constancy of Intermediate-Degree p-Mode Frequencies
    during the Declining Phase of Solar Cycle 21
Authors: Rhodes, Edward J., Jr.; Woodard, Martin F.; Cacciani,
   Alessandro; Tomczyk, Steven; Korzennik, Sylvain G.; Ulrich, Roger K.
Bibcode: 1988ApJ...326..479R
Altcode:
  A comparison of two sets of frequencies of intermediate-degree (6 ≤ l
  ≤ 89) solar p-mode oscillations obtained in late 1981 and in mid-1984
  shows agreement at the level of 0.02 μHz, or better than one part in
  10<SUP>5</SUP>. In particular, the frequencies of 573 modes obtained
  at the South Pole during 1981 December 24 - 25, (reported by Duvall,
  Harvey, and Pomerantz in 1987) were compared with the frequencies of
  the same modes as observed at the Mount Wilson Observatory 60 foot
  Solar Tower from 1984 July 29 through August 13. It is concluded that
  the data are consistent with no change in intermediate-degree p-mode
  frequencies between late 1981 and mid-1985.

Title: Estimates of the solar internal angular velocity obtained
    with the Mt. Wilson 60-foot solar tower
Authors: Rhodes, Edward J., Jr.; Cacciani, Alessandro; Woodard,
   Martin; Tomczyk, Steven; Korzennik, Sylvain; Ulrich, R. K.
Bibcode: 1987ASSL..137...75R
Altcode: 1987isav.symp...75R
  Estimates are obtained of the solar internal angular velocity from
  measurements of the frequency splittings of p-mode oscillations. A
  16-day time series of full-disk Dopplergrams obtained during July and
  August 1984 at the 60-foot tower telescope of the Mt. Wilson Observatory
  is analyzed. Power spectra were computed for all of the zonal, tesseral,
  and sectoral p-modes from l = 0 to 89 and for all of the sectoral
  p-modes from l = 90 to 200. A mean power spectrum was calculated for
  each degree up to 89. The frequency differences of all of the different
  nonzonal modes were calculated for these mean power spectra.

Title: Full-disk solar dopplergrams observed with a one megapixel
    CCD camera and sodium magnetooptical filter
Authors: Rhodes, Edward J., Jr.; Cacciani, Alessandro; Tomczyk, Steven
Bibcode: 1987ASSL..137...69R
Altcode: 1987isav.symp...69R
  The paper presents here the first two full-disk solar Dopplergrams
  obtained with the new 1024 x 1024-pixel CCD camera which has recently
  been installed at the 60-Foot Tower Telescope of the Mt. Wilson
  Observatory. These Dopplergrams have a spatial resolution of 2.2
  arcseconds and were obtained in a total of one minute of time. The
  Dopplergrams were obtained with a magnetooptical filter which was
  designed to obtain images in the two Na D lines. The filter and the
  camera were operated together as part of the development of a solar
  oscillations imager experiment which is currently being designed at JPL
  for the Joint NASA/ESA Solar and Heliospheric Observatory mission. Two
  different images obtained by subtracting two pairs of the Dopplergrams
  from the initial time series are also included.

Title: Applications of the magneto-optical filter to stellar pulsation
    measurements
Authors: Rhodes, Edward J., Jr.; Cacciani, Alessandro; Tomczyk, Steven
Bibcode: 1986ASIC..169..359R
Altcode: 1986ssds.proc..359R
  A proposed method of employing the Cacciani magneto-optical filter (MOF)
  for stellar seismology studies is described. The method relies on the
  fact that the separation of the filter bandpasses in the MOF can be
  changed by varying the level of input power to the filter cells. With
  the use of a simple servosystem the bandpass of a MOF can be tuned to
  compensate for the changes in the radial velocity of a star introduced
  by the orbital motion of the earth. Such a tuned filter can then be
  used to record intensity fluctuations through the MOF bandpass over
  an extended period of time for each given star. Also, the use of a two
  cell version of the MOF makes it possible to alternately chop between
  the bandpass located in the stellar line wing and a second bandpass
  located in the stellar continuum. Rapid interchange between the two
  channels makes it possible for atmospheric-introduced noise to be
  removed from the time series.

Title: A one-megapixel image acquisition and processing system for
    solar oscillation studies.
Authors: Rhodes, Edward J., Jr.; Bursch, Thomas K.; Ulrich, Roger K.;
   Tomczyk, Steven
Bibcode: 1986SPIE..627..256R
Altcode:
  The 1-Mpixel image acquisition and processing system that has been
  installed at the Mt. Wilson observatory as part of the development
  effort for the NASA/ESA Solar Oscillations Imager Experiment of the
  projected Heliospheric Observatory mission is discussed. The system
  encompasses a high speed CCD camera with a 1024 x 1024-pixel virtual
  phase chip array, yielding a readout rate of about 800,000 pixels/sec;
  this allows the entire Mpixel array to be read out in just over 1
  sec. The camera is interfaced with a floating point array processor
  that integrates several successive exposures from the CCD camera and
  differences selected pairs of integrated images. The system is currently
  being used to record and difference narrowband images of the sun.

Title: The 1984 solar oscillation program of the Mt. Wilson 60-foot
    tower.
Authors: Rhodes, Edward J., Jr.; Cacciani, Alessandro; Tomczyk,
   Steven; Ulrich, Roger K.
Bibcode: 1986ASIC..169..309R
Altcode: 1986ssds.proc..309R
  The authors describe the instrumentation, data, and preliminary results
  from the summer, 1984, solar oscillation observing program which
  was carried out using the 60-foot tower telescope of the Mt. Wilson
  Observatory.

Title: Non-radial pressure mode oscillations as a seismic probe of
    solar structure
Authors: Rhodes, Edward Joseph, Jr.
Bibcode: 1977PhDT.......159R
Altcode:
  No abstract at ADS

