The Solar Maximum Mission support program is mentioned along with investigations of the solar corona, prominences, and chromosphere. The solar limb was studied using far infrared and submillimeter photometry. Stokes profiles obtained from sunspot observations were examined with a polarimetric technique

Hall, D. N. B.

Landman, D. A.

Orrall, F. Q.

English

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NASA STI FACILITY
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NASA GRANT NGL 12-001-011
Semiannual Status Report
CORONAL AND CHROMOSPHERIC PHYSICS
UNIVERSITY OF HAWAII
INSTITUTE FOR ASTRONOMY
2680 Woodlawn Drive
Honolulu, Hawaii 96822
Donald N. B. Hall, Principal Investigator
Donald A. Landman, Co-Investigator
Frank Q. Orrall, Co-Investigator
For the Period
May 1, 1984 - October 31, 1984
2A. Solar Maximum Mission Support Program
Our ground-based synoptic support program for the revived Solar Maximum
Mission satellite has been in operation since the restart of spacecraft
observations. In this connection we have built and installed two new
microcomputer-based camera controllers for the dual coronagraph (Ha, Fe XIV
X5303) and tunable narrow-band Zeiss Ha systems. These instruments, together
with the Stokes polarimeter and K-Line Filtergraph, are run in routine support
of current SMM programs on an ongoing basis. More specialized data are
obtained by interested staff scientists in collaboration with SMM experiment
team members on projects of mutual scientific interest.
B. Solar Activity
M. McCabe (with D. G. Same and C. J. Garcia [HAO]) carried out an objec-
tive statistical comparison of bright features higher than 1.3 Ro
 in the
corona and neutral lines in the photcspheric field seen at X6303. Some corre-
lation was fount; but not a unique and prevailing relationship. Many coronal
features are associated with specific neutral lines, but the conditions that
are necessary sn^ sufficient are not yet identified. They are continuing this
investigation by identifying individual neutral lines and prominences and
looking for any related coronal feature and vice versa.
Observations at Haleakala are continuing in support of SMM II. Solar
activity has been very low, but we have Ha and X5303 data on several promin-
ences and surges and at least one eruptive event is known to correlate with a
C/P transient. Observations of the filaments and filament channels, as well.
as magnetograms of active regions have been recorded in an attempt to obtain
simultaneous data with the UVSP experiment. We plan to compare and collate
their data at the next meeting on Prominence and Coronal Plasmas at Goddard in
April 1985. In October a joint program was initiated to obtain concurrent
measurements of Ha (Haleakala) and La (UVSP) ir.t:egrated intensities and
profiles of prominences to test theoretical modeling of the hydrogen excita-
tion including the importance of partial redistributi3n effects.
McCabe completed the study of the Ha manifestatian on a gamma-ray flare
event at the limb on 21 June 1980 (SMM I).
C. Prominence and Chromospheric Studies
During this grant period, Landman has continued work on his program of
prominence and spicule spectral analysis. This effort has led to the estab-
lishment of a powerful and practicable method of plasma diagnostics for the
cool parts of these objects. Using measurements of the resonance lines of Na,
Mg (triplet system), and Sr+ , together with the middle H Balmer or Paschen
lines, we are able to determine the basic parameters: temperature, microturb-
ulence, vertical flare velocity, electron density, degree of hydrogen ioniza-
tion, and line-of-sight thickness of the emitting region. Using data obtained
at Haleakala and elsewhere, we have applied this method to evaluating condi-
tions in quiescent prominences and spicules, and this work has been reported
in several Astrophysical Journal articles. A result of major significance is
the relatively low degree of hydrogen ionization that obtains in these
3features (-107), so that with our value of ne - 1011 cm-3, the total gas pres-
sure is about an order of magnitude greater than that of the neighboring
corona. Our most recent study along these lines involves a comparison of Sr+
and Ba+
 resonance line intensities to estimate the internal H Lya flux. This
work also includes new calculations of the Sr + and Ba+ oscillator strengths
and photoionization cross sections with spin-orbit and core polarization
effects taken into account.
Landman has also completed a study of the small-scale nonthermal velocity
field in quiescent prominences using simultaneous, high-precision measurements
of the Mg XX5173,5167 and Fe + X5169 lines obtained at daleakala. We find that
the Fe+
 line is systematically narrower than would be expected from the
corresponding Mg line widths and the assumption of a common temperature and
microturbulence parameter for both constituents. The detailed behavior of
this new effect apparently implies a systematic decrease in the Fe + micro-
turbulence parameter compared to that for Mg, which suggests the presence of
some type of magnetic rigidity phenomenon acting selectively on the ionic
component.
Continuing his series of calculations on proton impact excitation in
transition region and coronal ions, Lai.dman is completing work on transactions
among the 2p 5 3s configuration levels of the Ne isoelectronic sequence ions
Na II-Ni XIX.
D. Far-Infrared and Submillimeter Photometry
C. Lindsey is continuing analysis of far-infrared observations made from
the Kuiper Airborne Observatory (KAO) in t`he total solar eclipse of 31 July
1981 with Becklin, Jefferies, Orrall, Werner, and Gatley. He has computed the
extreme limb brightness profiles of the Sun in 30, 50, 100 and 200 um
radiation from observations of occultation of the solar limb during eclipse.
The results are published in the proceedings of the Airborne Astronomy
Symposium (Becklin et al. 1984). Results of a more detailed analysis are
being prepared for publication in The Astrophysical Journal.
Lindsey and graduate student L. Hermans have completed a project on
chromospheric modeling independent of the assumption of gravitational-
hydrostatic equilibrium based on the far-infrared limb profiles discussed
above. This work is the subject of Herman's recently completed thesis, and is
being prepared for publication in The Astrophysical Journal.
Lindsey is working with graduate student E. Pilger on analysis of exten-
sive two-beam infrared scans of the Sun made from both the KAO and the NASA
Infrared Telescope Facility (IRTF). The results of this analysis will yield
maps of the Sun useful for studying active region brightness dependence on
distance from the solar limb.
Lindsey is working with T. Roellig (NASA-Ames Research Center) on a proj-
ect to use the IRTF to study continuum solar variations in several submilli-
meter bands concurrently. Roellig has constructed a photometer especially for
this purpose, originally designed for eclipse observations from 'he KAO. They
are preparing optical components to adapt this system to the IRTF. This is a
continuation of work started by Lindsey and Kaminski (1984).
;E
K
4E. Coronal and Transition Region Studies
In a continuing collaborative program of EUV spectrophotometry with G. J.
Rottman of the Laboratory for Atmosp;.eric and Space Physics (LASP), Orrall
took part in a successful flight of the LASP rocket-borne EUV Coronal
Spectrometer from White Sands on 19 June 1984. Co-pointed with the spectrom-
eter was an XUV broad-band imaging telescope that employs a 32 x 32 Codacon
defector. As the SPARCS guiding system scanned the spectrometer and imaging
telescope back and forth along a solar diameter, XUV images of a strip of the
Sun 10 arcmin wide were formed. Both the spectrometer and imaging telescope
returned good data. First order reduction of both data sets has now been
completed. The data set includes observations of active regions, quiet Sun,
Coronal holes, and a prominence.
In a collaborative program with the SMM experimenters, SMM observations
were obtained on the day of the flight along the entire strip of the Sun
studied by the rocket-borne instruments. A comparative study of data obtained
with the SMM Flat Crystal Spectrometer and the XUV imaging spectrometer is in
progress.
There has been a long-standing discrepancy between models of the corona
based on EUV data and models based on radiD data. To obtain the necessary
co-spatial and co-temporal observations at EUV nr ►d centimetric wavelengths,
Orrall and Rottman, together with G. Dulk and T. Bastian (U. Colorado),
obtained observing time on the VLA and at Greenbank on 19 June 1984, the day
of the rocket flight. Successful observations were obtained, and the second
order cleaning of the maps is being carried out by Dulk and Bastian.
Similarly, M. Kundu (U. Maryland) obtained radio maps at several metric
wavelengths on the same day from Clark Lake.
Orrall and Rottman have had a continuing collaboration with R. Fisher and
R. Munro (HAO/NCAR) to make an absolute photometric comparison of the
K-Coronal brightness pB with the EUV emission line corona. Co-spatial and
co-temporal observations of pB were made successfully from Mauna Lob with
HAO's Mark III K-coronameter during flights of the LASP EUV Spectrometer in
1980, 1983, and 1984. The combined analysis of this data has been ccmpleted.
One important result is that the inner corona is more irregular on small scale
than was previously known. A paper for Tne " Q trophysical Journal is in
preparation, and an abstract describing results was submitted for the January
AAS meeting.
F. Stokes Polarimetry and Magnetic Fields
D. Mickey attended a workshop on measurements of solar vector magnetic
fields at Marshall Space Flight Center (MSFC) in May.
Mickey is studying Stokes profiles obtained from sunspot observations
with the Haleakala polarimeter in order to understand the net circular
polarizations obtained when sunspots are observed in broad wavelength bands.
Haleakala observations were obtained for one of the spots described by Henson
and Kemp (1984, Solar Phys. 93, 289), and integrals over our line profiles
give similar results: a net polarization of one sign in the penumbra, with a
reversal in the umbra. Specifically, our sunspot maps show a net polarization
5with the same sign as the spot magnetic field in the penumbra at points where
the magnetic field is nearly transverse to the line of sight. In the umbra,
the net polarization is almost as large, but in the opposite sense. Mickey is
analyzing observations of other spots and different spectral lines to
determine the generality of this behavior.
The polarimeter has also been used to obtain Stokes profiles of a single
spot in several spectral lines, formed at different heights in the solar
atmosphere to test magnetic field predictions of sunspot models.
Mickey has participated in collaborative projects with M. Hagyard and E.
West at MSFC, designed to obtain near-simultaneous vector magnetograms of the
same region with the Haleakala polarimeter and the Marshall magnetograph—and
in one attempt, the SMM UVSP as well. Some success was achieved with the
ground-based instru!ients, particularly a series of observations of NOAA region
4474 in late April and early May. The combination of the data sets should
give useful information on the relation calibrations of the two instruments,
as well as providing more complete data on evolution of the magnetic field in
this region.
There has been some indication of a 13-day periodicity in global solar
velocity measurements by the Birmingham group. To investigate the effect of
plage and spot regions on the X7699 global velocity observations, Mickey has
made several Stokes spectroheliograms in this line.
G. Publications
The following publications pertinent to this grant were published during
1984, were accepted or submitted for publication, or are presently being
edited for publication:
Becklin, E. E., Lindsey, C., Jefferies, J. T., Orrall, F. Q., Werner, M., and
Gatley, I. 1984. Extreme Limb Profiles of the Sun at Far Infrared and
Submillimeter Wavelengths. Proceedings of the Airborne Astronomy
Symposium, NASA-Ames Research Center, in press.
Bruning, D. H., and LaBonte, B. J. 1984. Integrated Light Observations of
the Asymmetry of the X5250 Line. Tn Conference on Small-scale Dynamics
of Stellar Atmospheres, Sacramento Peak, in press.
Fisher, R., McCabe, M., Mickey, D., Seagraves, P., and Sime, D. G. 1984. The
Sun as a Star: 14 June-13 August 1982. Ap. J., 280, 873.
Foukal, P., and Landman, D. A. 1985. Interpretations of Electric Fields in
Coronal Magnetic Loops. IAU Colloquium No. 86, Washington, DC, in press.
Gergeley, T. E., Kundo, M. R., Erskine, F. T., III, Sawyer, C., Wagner,
W. J., Illing, R., House, L. L., McCabe, M. K., Stewart, R. T., Nelson,
G. J., Koomen, M. J., Michels, D., Howard, R., and Sheeley, N. 1984.
Radio and Visible Light Observations of a Coronal Arcade Transient.
Solar Phys., 90, 161.
Hermans, L. 1984. Modeling the Solar Chromosphere Based on Submillimeter
Limb Profiles, M.S. Thesis, University of Hawaii, Honolulu.
6LaBonte, B. J. 1984. Is Stellar Differential Rotation Observable? Ap. J.,
276, 335.
LaBonte, B. J. 1984. On Measuring Solar Torsional. 0s-:illation Using Sunspot
Motions. Astr. Ap., 135, 175.
LaBonte, B. J. 1984. Recent Ground-Based Observations of the Global
Properties of the Sun. In Solar Irradiance Variations on Active Region
Timescales, B. J. LaBonte, G. A. Chapman, H. S. Hudson, and R. C.
Willson, eds. NASA Conference Publication 2310.
LaBonte, B. J. 1984. Ha as a Stellar Diagnostic, in preparation.
LaBonte, B. J., Chapman, G. A., Hudson, H. S., and Willson, R. C., eds. 1984.
Solar Irradiance Variations on Active Region Timescales, NASA Conference
Publication 2310.
LaBonte, B. J., and Rose, J. A. 1984. Magnetic Plages and the Hyades
Anomaly, in preparation.
Landman, D. A. 1984. Physical Conditions in the Cool Parts of Prominences
II. The Mg Triplet Lines. Ap. J-, 279, 438.
Landman, D. A. 1984. Physical Conditions in the Cool Parts of Spicules.
Ap. J., 284, 833.
Landman, D. A. 1985. Physical Conditions in the Cool Parts of Prominences.
III. The Sr+/Ba+ Resonance Line Ratios and the Internal Lyu Flux.
Ap. J., in press.
Landman, D. A. 1985. A Spectral Analysis of the Low Temperature Material in
Spicules. In Proceedings of the Workshop on Chromos heric Diagnostics
and Modelling 13-16 August 1984), B. W. Lites, ed.	 Sunspot: National
Solar Observatory/Sacramento Peak), in press.
Landman, D. A. 1985, A New Property of the Small-Scale Non-Thermal Motions in
Quiescent Prominences. Ap. J., submitted.
Lindsey, C., Becklin, E. E., Hermans, L., Jefferies, J. T., Orrall, F.,
Gatley, I. I., and Werner, M. W. 1984. A Determination of the
Submillimeter Brightness Profile of the Extreme Solar Limb from
Observations of the Eclipse of 1981 July 31, in preparation.
Lindsey, C., Becklin, E. E., Jefferies, J. T., Orrall, F. Q., Werner, M. W.,
and Gatley, I. 1984. Observations of the Brightness Profile of the Sun
in the 30-200 Micron Continuum. Ap. J., 281, 862.
Lindsey, C., de Graauw, Th., de Vries, C., and L!.dholm, S. 1984. Solar Limb
Brightening at 820 Microns. Ap. J., 277, 424.
Lindsey, C., and Kaminski, C. 1984. Temporal Variations in the Solar
Submillimeter Continuum. Ap. J. Lett., 282, L106.
McCabe, M. K. 1984. Ha Manifestation of an Energetic Gamma Ray Event at the
Solar Limb. Solar Phys., submitted.
7Orrall, F. Q., Rottman, G. J., Fisher, R. R., and Munro, R. 1985. A
Photometric Comparison of EUV- and K-coronas. Ap. J., in preparation.
Pasachoff, J. M., and Landman, D. A. 1984. High-Frequency Coronal
Oscillations and Coronal '.eating. Solar Phys., in press.
Sime, D. G., Fisher, R. R., McCabe, M. K., and Mickey, D. L. 1984. The
Co-ona Near the Time of the 1983 June 11 Total Solar Eclipse. Ap. J.
Lett., 278, L123.
Strong, K. T., Smith, J. B., McCabe, M., Machado, M., Saba, J. L. R., and
Simnett, G. M. 1984. Homologous Flares aLl the Evolution of NOAA-Region
2372. Advances in Space Research, submitted.
Woodgate B. E., Martres, M. J., Smith, J. B., Strong, K. T., McCabe, M. K.,
Machado, M. E., Gaisauskas, V., Stewart, R. T., and Sturrock, P. A.
1984. Progress in the Stddy of Homologous Flares on the Sun. Advances
in Space Research. Proc. of 25th Plenary Meeting of COSPAR, Austria,
1984, submitted.
The following are abstracts of papers presented or to be presented to the
American Astronomical Society or the American Geophysical Union:
Garcia, C. J., Sime, D. G., and McCabe, M. K. 1984. Photospheric Magnetic
Fields and the White Light. B.A.A.S., 16, 533.
Landman, D. A. 1984. Physical Conditions in the Cool Parts of Spicules.
B.A.A.S., 15, 970.
Landman, D. A. 1984. Conditions in Solar Prominences: Relative Ba+/°r+ Line
Intensities and the Internal Lya Flux. B.A.A.S., 16, 531.
Landman, D. A. 1984. On Helium Excitation in Quiescent Prominences.
B.A.A.S., 16, 1004.
Lindsey, C., Becklin, E. E., Orrall, F. Q., Werner, M. W., Jefferies, J. T.,
Gatley, I. 1984. Extreme Limb Profiles of the Sun at Far-Infrared and
Submillimeter Wavelengths. B.A.A.S., 16, 992.
Orrall, F. Q., Rottman, G. J., Fisher, R. R., and Munro, R. 1985. B.A.A.S.,
in press.
Yasukawa, E. A., Sime, D. G., and McCabe, M. K. 1984. EOS Trans., 65, 1071.


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