A model of the spectrum of the slowly varying component of solar radio emission from active regions

Details A model of the spectrum of the slowly varying component of solar radio emission from active regions A model of the spectrum of the slowly varying component of solar radio emission from active regions

Jun 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982acasn..23..309y&link_type=abstract

(Acta Astronomica Sinica, vol. 23, no. 4, 1982, p. 309-316) Chinese Astronomy and Astrophysics (ISSN 0275-1062), vol. 7, June 19

Astronomy and Astrophysics

Astrophysics

2

Centimeter Waves, Solar Flares, Solar Magnetic Field, Solar Protons, Solar Radio Emission, Solar Spectra, Sunspots, Gyrofrequency, Magnetic Flux, Magnetic Resonance, Particle Acceleration, Radio Spectra, Solar Corona, Solar Flux, Solar Temperature

Scientific paper

Reference is made to statistical analyses of solar radio observations showing that proton events are likely to occur when the flux at 3 cm, S3, of the slowly varying component (SVC) exceeds 25 sfu and when the ratio of S3 to S8 (the flux at 8 cm) is greater than unity. The study presented here provides a theoretical explanation of this. The spectrum of the SVC is calculated using the gyro-radiation emission, and it is found that the main reason for S3 being greater than 25 sfu is a tenfold increase in the conductive energy flux in the active region over the quiet region; this raises the height of the gyro-resonance layer for the 3-cm emission. It is also found that the main reason that the the S3/S8 ratio is greater than or approximately equal to 1 is an increase in the coronal magnetic field gradient in the active region, causing a decrease in the optical thickness for the gyro-resonance absorption at 3 cm. It is precisely these active regions that are most conducive to the production of proton events.

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