Generation of Type III Solar Radio Bursts in the Low Corona by Direct Amplification. II. Further Numerical Study

Details Generation of Type III Solar Radio Bursts in the Low Corona by Direct Amplification. II. Further Numerical Study Generation of Type III Solar Radio Bursts in the Low Corona by Direct Amplification. II. Further Numerical Study

Sep 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002apj...576..552y&link_type=abstract

The Astrophysical Journal, Volume 576, Issue 1, pp. 552-560.

Astronomy and Astrophysics

Astronomy

13

Methods: Numerical, Sun: Corona, Sun: Radio Radiation

Scientific paper

In a recent paper a cyclotron maser model was proposed as an alternative explanation of coronal type III solar radio bursts. However, the discussion was preliminary in that it was limited to a local theory and in that the propagation of the emitted waves was studied with a simplified scheme. The present article complements the earlier study by simultaneously computing the ray trajectory with a more sophisticated approach and estimating the intensity of the amplified waves. Numerical results lead to the conclusion that the O1-mode is insignificant despite the robust initial growth rate predicted by local theory, while X1- and X2-modes are equally important. This finding is consistent with observations and confirms the scenario originally put forward in the earlier paper.

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