Shock accelerated electron beams in the solar corona

Details Shock accelerated electron beams in the solar corona Shock accelerated electron beams in the solar corona

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.506..245m&link_type=abstract

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

Physics

9

Electron Acceleration, Shock Waves, Solar Radio Radiation

Scientific paper

In the solar corona shock waves can be produced by flares and/or coronal mass ejections. Type II radio bursts represent the signature of such shock waves in the solar radio radiation. Shock accelerated electron beams appear as rapidly drifting emission stripes (so-called "herringbones") within type II radio bursts. A large sample of "herringbones" and solar type III radio bursts is statistically analysed concerning their properties in dynamic radio spectra. Type III bursts are regarded as being associated with electron beams immediately generated by the flare process. The analysis shows that the drift rates of "herringbones" are significantly smaller (about one half) than those of type III bursts in the same frequency range. Thus, electron beams related to type III bursts have a higher velocity than those generated by coronal shock waves. The velocity of electron beams associated with "herringbones" is found to be about 30,000 km/s. These beams are considered to be produced by shock drift acceleration. Then, the accelerated electrons establish a shifted loss-cone distribution in the upstream region of the associated shock wave. Such a distribution leads to a plasma instabilities leading to the emission of radio waves as observed as "herringbones".

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