The magnetic field in the corona above sunspots at the eclipse of 1991 July 11

Details The magnetic field in the corona above sunspots at the eclipse of 1991 July 11 The magnetic field in the corona above sunspots at the eclipse of 1991 July 11

Jul 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...412..421g&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 412, no. 1, p. 421-430.

Astronomy and Astrophysics

Astrophysics

11

Solar Corona, Solar Eclipses, Solar Magnetic Field, Sunspots, Brightness Temperature, Emission Spectra, Field Strength, Photosphere, Radio Spectra, Solar Arrays, X Ray Imagery

Scientific paper

A partial solar eclipse and an X-ray image are used to study the magnetic field as a function of height in the corona above an active region during the solar eclipse of July 11, 1991. The dominant features of AR 6718 are two leading spots of positive polarity followed by two spots of negative polarity about 3 arcmin to the east. Bright radio emission coincides with the positions of the sunspots, attributable to a gyroresonance radiation from ambient electrons above the spots. A simplified model of the source as a function of frequency based on the interferometer fringe amplitudes is used to obtain brightness temperature spectra for the emission associated with the sunspots. It is deduced that the magnetic field strength at the base of the corona above the leading spots was 1200 G, and about 1100 G above the following spots. The soft X-ray brightness above the sunspots was very low, about 30 times lower than that of the adjacent plage-associated emission.

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