Type II radio emission in coronal transients

Details Type II radio emission in coronal transients Type II radio emission in coronal transients

Aug 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984soph...94..193s&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 94, Aug. 1984, p. 193-202.

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Coronal Loops, Solar Corona, Type 2 Bursts, Computational Astrophysics, Propagation Velocity, Shock Waves, Solar Flares, Transient Response

Scientific paper

Meter wavelength type II radio emission in the corona is generally considered indicative of a shock wave. Wagner and MacQueen (1983) have provided an explanation of the trailing type II radio emission which suggests that the transient is initiated prior to a flare shock which produces the type II burst. The flare shock travels faster than the transient and may eventually overtake it. In this model, type II bursts result when the flare shock interacts with the compressed lateral sides of the loop-shaped transient. The present investigation is concerned with an alternate interpretation of the present data. The approach considered employs a suggestion, made by Holman and Pesses (1983), that the shock drift acceleration of electrons acts as a precursor to type II emission. Attention is given to the observations, the coronal transient model, and the type II emission model.

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