Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...434..786s&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 434, no. 2, p. 786-794
Astronomy and Astrophysics
Astronomy
29
Brightness Temperature, Circular Polarization, Electron Energy, Magnetic Field Configurations, Magnetic Signatures, Radio Astronomy, Solar Corona, Stellar Models, X Ray Astronomy, X Ray Spectra, Calcium, Iron, Magnesium, Neon, Oxygen, Radio Interferometers, Solar Maximum Mission, Spectrometers, Very Large Array (Vla), X Ray Telescopes
Scientific paper
Simultaneous soft X-ray, microwave, and photospheric magnetic field observations were taken during the Coronal Magnetic Structures Observing Campaign (CoMStOC '87). The plasma electron temperature and emission measures determined from the X-ray data are used to predict the free-free emission expected at 20 and 6 cm. Comparing these predictions with the microwave observations, it is found that the predicted 20 cm brightness temperatures are higher than the observed, requiring cool absorbing material between the hot X-ray plasma and the observer. The model that is most consistent with all the observations and minimizes the required coronal fields indicates that this 20 cm emission is either free-free or a combination of free-free and fourth harmonic cyclotron emanating from the X-ray plasma with an electron temperature of approximately 3.1 x 106 K and an emission measure of approximately 1.3 x 1029/cm5. The observed 20 cm polarization requires a field strength of greater than or equal to 150 G. In addition, the 6 cm emission is free-free, emanating from cooler plasma with an electron temperature of approximately 1.5 x 106 K and an emission measure of approximately 3-6 x 1029/cm5. This model is consistent with the rather unusual combination of high 20 cm and low 6 cm polarization as well as the low extrapolated coronal fields.
Brosius Jeffrey W.
Holman Gordon D.
Schmelz Joan T.
Willson Robert F.
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