Physics
Scientific paper
Mar 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989soph..121..449z&link_type=abstract
(IAU, Colloquium on Solar and Stellar Flares, 104th, Stanford, CA, Aug. 15-19, 1988) Solar Physics (ISSN 0038-0938), vol. 121, n
Physics
12
Cyclotron Radiation, Line Spectra, Solar Flares, Solar Spectra, Brightness Temperature, Nonuniform Magnetic Fields, Solar Magnetic Field, Temperature Distribution
Scientific paper
A cyclotron line-like solar spectrum was observed by Willson (1985) using the VLA at 10 closely-spaced frequencies near 20 cm. This paper interprets this observation on the basis of an active region model in which thermal cyclotron radiation is produced by hot plasma filling the magnetic tube in the corona above a group of spots. In this model, the frequency of the recorded 1658 MHz line corresponds to the third harmonic of electron gyrofrequency, which yields the magnetic field along the magnetic tube axis. The linewidth is determined by the 10 percent inhomogeneity of the magnetic field over the tube cross section. The line profile indicates the kinetic temperature distribution of electrons over the tube cross section with the maximum value of 4 x 10 to the 6th K.
Zhelezniakov Vladimir V.
Zlotnik Ia. E.
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