The measurement of magnetic fields in the solar atmosphere above sunspots using gyroresonance emission

Details The measurement of magnetic fields in the solar atmosphere above sunspots using gyroresonance emission The measurement of magnetic fields in the solar atmosphere above sunspots using gyroresonance emission

Jul 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982soph...79...41a&link_type=abstract

Solar Physics, vol. 79, July 1982, p. 41-58.

Physics

62

Magnetic Measurement, Solar Atmosphere, Solar Magnetic Field, Solar Radio Emission, Solar Spectra, Sunspots, Centimeter Waves, Chromosphere, Circular Polarization, Solar Corona, Temperature Distribution

Scientific paper

The presence of a core component characterized by strong circular polarization and a steeply growing spectrum at the shorter cm wavelengths, and coinciding in position with the umbra of the sunspots at a photospheric height of less than about 2000 km, is confirmed by an analysis of the local sources (LS) structure of the solar radio emission S-component. By determining the short wavelength limit of LS gyroresonance emissions, and relating it to the third gyrofrequency harmonic, the maximum magnetic fields of the corresponding sunspots at the height of the chromosphere-corona transition region (CCTR) can be measured. An analysis of a large number of sunspots and their LS has shown a good correlation between radio magnetic fields near the CCTR and optical photospheric ones. The CCTR magnetic field above a sunspot is only 10-20% lower than in the photosphere, and the resulting field gradient is not less than 0.25 G/km.

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