Model of Gyrosynchrotron Emission from a High Coronal Loop

Details Model of Gyrosynchrotron Emission from a High Coronal Loop Model of Gyrosynchrotron Emission from a High Coronal Loop

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...180.4205k&link_type=abstract

American Astronomical Society, 180th AAS Meeting, #42.05; Bulletin of the American Astronomical Society, Vol. 24, p.796

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Scientific paper

Gyrosynchrotron emission is a main source of microwave emission from solar flares. We have developed a model of a high, face-on, coronal flare loop with a dipole magnetic field. The loop is divided into homogeneous segments to which are applied a general gyrosynchrotron code. We compare the model with observations made of an off-limb flare taken in June of 1989 during the first Max '91 campaign. These observations force a strong set of constraints upon the model. VLA imaging data at 1.4 GHz dictate the source position, shape and brightness at that frequency. Radiometer data from RSTN and Bern provide microwave spectra to compare to model-produced spectra, and there are constraints from SMM/HXRBS hard X-ray spectra and derived emission measures. The model is also compared with general results from previous measurements of source parameters at other frequencies.

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