Formation Of Coronal Mhd Shock Waves - I. The Basic Mechanism

Details Formation Of Coronal Mhd Shock Waves - I. The Basic Mechanism Formation Of Coronal Mhd Shock Waves - I. The Basic Mechanism

Sep 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000soph..196..157v&link_type=abstract

Solar Physics, v. 196, Issue 1, p. 157-180 (2000).

Physics

45

Scientific paper

The formation and evolution of a large amplitude MHD perturbation propagating perpendicular to the magnetic field in a perfectly conducting low β plasma is studied. The perturbation is generated by an abrupt expansion of the source region. Explicit expressions for the time and the distance needed for the transformation of the perturbation's leading edge into a shock wave are derived. The results are applied to coronal conditions and the dynamic spectra of the radio emission excited by the shock are synthesized, reproducing metric and kilometric type II bursts. The features corresponding to the metric type II burst precursor and the moving type IV burst in the case of kilometric type II bursts are identified. A specific radio signature that is sometimes observed at the onset of a metric type II burst is found to appear immediately before the shock wave formation due to the associated growth of the magnetic field gradient. Time delays and starting frequencies of bursts' onsets are calculated and presented as a function of the impulsiveness of the source-region expansion, using different values of the ambient Alfvén velocity and various time profiles of the expansion velocity. The results are confronted with the observations of metric and kilometric type II solar radio bursts.

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