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Bidirectional Type III Solar Radio Bursts View all abstracts by submitter

Arnold Benz   Submitted: 1999-11-04 13:02

Bidirectional coronal type III bursts are modeled by combining a model of coronal electron heating and beam generation via time-of-flight effects with semiquantitative estimates of quasilinear relaxation. Electromagnetic emissivit- emissivities are estimated by extending the recently developed theory of interplanetary type III bursts to coronal emissions, including its features of stochastic Langmuir-wave growth and three-wave interactions. The results are investigated for heating on open and closed coronal field lines and are compared with observations of normal, reverse-slope, bidirectional, and inverted-J and -U coronal type III radio bursts. Harmonic emission is predicted to dominate at plasma frequencies above roughly 100 MHz where the efficiency of fundamental emission falls off steeply, while its free-free reabsorption rises. The model also explains the observed trends in the likelihood of occurrence of normal, reverse-slope, and bidirectional coronal type III bursts.

Authors: P. A. Robinson and A. O. Benz
Projects: None

Publication Status: Solar Physics, 194, 371 - 391 (2000)
Last Modified: 2005-11-17 01:40
Go to main E-Print page  Particle Acceleration at the Sun and in the Heliosphere
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