Physical conditions in the reconnection outflow

Details Physical conditions in the reconnection outflow Physical conditions in the reconnection outflow

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.506..757s&link_type=abstract

In: Solar variability: from core to outer frontiers. The 10th European Solar Physics Meeting, 9 - 14 September 2002, Prague, Cze

Physics

1

Sun, Flares, Mhd, Reconnection

Scientific paper

The amplitude of the standing fast mode shock formed in the reconnection outflow is studied. The dependence on the Mach number of the inflow, the direction of the inflow, the transversal magnetic field, and the plasma to magnetic pressure ratio is investigated in 2-D and 2 1/2-D model separately. The results are presented stressing the observable quantities such as the band-split of the radio emission excited in the upstream and downstream regions of the fast mode shock. For the range of parameter values appropriate for the occurrence of solar flares it is found that the relative band-split should be in the range 10-50%.

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