Models of gamma-ray production in solar flares

Details Models of gamma-ray production in solar flares Models of gamma-ray production in solar flares

Sep 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988aipc..170..217r&link_type=abstract

AIP Conference Proceedings, Volume 170, pp. 217-227 (1988).

Physics

9

Scientific paper

We review gamma-ray production models in solar flares and study the transport of ions and relativistic electrons by employing a Monte-Carlo simulation that follows the individual particles throughout a flare loop. We consider energy losses, magnetic mirroring, MHD pitch-angle scattering, turbulence damping, Coulomb scattering, and drifts. For an isotropic injection of particles, MHD pitch-angle scattering in the corona could account for the rapid variability of the observed gamma-ray time profiles. Owing to damping by neutral hydrogen, such pitch-angle scattering is probably negligible in the chromosphere. Therefore, magnetic mirroring in convergent flux tubes in the chromosphere and upper photosphere is probably the dominant mechanism for producing both the anisotropies suggested by the preferential detection of >~10 MeV emission from flares near the solar limb and ultrarelativistic electron bremsstrahlung observed from flares on the disc.

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