On the proton origin of a small optical gamma-ray solar flare

Details On the proton origin of a small optical gamma-ray solar flare On the proton origin of a small optical gamma-ray solar flare

Jun 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...341..506r&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 341, June 1, 1989, p. 506-515. Research supported by the University of New

Astronomy and Astrophysics

Astronomy

4

Gamma Ray Astronomy, Shock Waves, Solar Flares, Stellar Models, Magnetic Field Configurations, Protons, Solar Corona, Solar Magnetic Field, Solar Radio Emission, Solar X-Rays

Scientific paper

The starting conditions for a small optical gamma-ray flare are examined, proposing a new scenario for the onset and development of a solar flare in which the starting or preflare conditions are critical to proton acceleration resulting in gamma-ray emission. It is suggested that the energy release in a gamma-ray flare is not a simple impulsive event but rather the result of an episodic process lasting for timescale of 1000 s. Eventually the release reaches a point where there is enough energy transferred to nonthermal ions so that a large chromospheric response is generated, which is observed as the flare. By means of shocks, the flare energy is converted into kinetic energy of nonthermal particles. The protons dominate the accelerated particle population energetically. In a gamma-ray flare, protons accelerated in the early stages are retained in the corona, acting as seed particles for further acceleration. The flare of 1042 UT on June 29, 1980 is used to illustrate these points.

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