Generation of Type III Solar Radio Bursts in Low Corona by Direct Amplification

Details Generation of Type III Solar Radio Bursts in Low Corona by Direct Amplification Generation of Type III Solar Radio Bursts in Low Corona by Direct Amplification

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsh22a..04y&link_type=abstract

American Geophysical Union, Spring Meeting 2002, abstract #SH22A-04

Physics

7509 Corona, 7514 Energetic Particles (2114), 7524 Magnetic Fields, 7534 Radio Emissions, 2159 Plasma Waves And Turbulence

Scientific paper

An alternative scenario to the plasma emission model is proposed for coronal type III solar radio bursts. According to this model, the radio bursts are produced inside a magnetic flux tube with density depletion, by a direct amplification of electromagnetic waves with frequencies near the electron gyrofrequency and its harmonics. The amplification mechanism is the cyclotron-maser instability driven by a beam of flare-generated streaming electrons. The propagation of an amplified wave is initially confined within the magnetic flux tube until the wave arrives at a point where the local exterior cutoff frequency is equal to the exiting wave frequency. The proposed model is spurred by the consideration that above an active region where the emission is presumed to originate, the ambient magnetic field is strong such that, in contrast to the conventional theories, it cannot be ignored. Numerical analysis leads to some encouraging results, on the basis of which we may resolve a number of longstanding issues raised by observations. The proposed scenario also implies a fundamentally different interpretation of the observed frequency drift in the dynamic spectrum.

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