Solar flares and shock waves

Details Solar flares and shock waves Solar flares and shock waves

Oct 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983s%26t....66..285m&link_type=abstract

Sky and Telescope (ISSN 0037-6604), vol. 66, Oct. 1983, p. 285-288.

Other

Computerized Simulation, Shock Waves, Solar Corona, Solar Flares, Coronal Loops, Solar Magnetic Field, Stellar Models, Type 2 Bursts

Scientific paper

Large-scale phenomena observed in the outer corona during a solar flare event are described, together with computer simulations of flare events. The events, which last from 30 sec to 5 min, expel matter at about 500 km/sec velocity, thereby also generating a shock wave ahead of the matter.The shock is a fast-moving magnetic disturbance, and matter moving less than 200 km/sec behind it will fall back to the sun. The leading edges of flare loops in the corona can expand upwards of 1000 km/sec. Protons and other heavy particles cause interplanetary high-energy particle storms, while outward bound electrons produce the Type II radio bursts, narrow, high-frequency bands of intense radio noise that drifts towards lower frequencies. Various emission frequencies have been correlated with specific distances above the solar surface. Computer simulations of events are run in up to three dimensions, with inputs being the energy, density, temperature, particle velocity, and magnetic field structures.

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