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Gamma-rays from Solar Flares

Published online by Cambridge University Press:  25 May 2016

R. Ramaty  and
N. Mandzhavidze
R. Ramaty
Affiliation:
NASA/GSFC, Greenbelt, MD 20771, U.S.A.
N. Mandzhavidze
Affiliation:
NASA/GSFC and USRA, Greenbelt, MD 20771, U.S.A.

Abstract

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Gamma-ray emission is the most direct diagnostic of energetic ions and relativistic electrons in solar flares. Analysis of solar flare gamma-ray data has shown: (i) ion acceleration is a major consequence of flare energy release, as the total flare energy in accelerated particles appears to be equipartitioned between ≳ 1 MeV/nucleon ions and ≳ 20 keV electrons, and amounts to an important fraction of the total energy release; (ii) there are flares for which over 50% of the energy is in a particles and heavier ions; (iii) in both impulsive and gradual flares, the particles that interact at the Sun and produce gamma rays are essentially always accelerated by the same mechanism that operates in impulsive flares, probably stochastic acceleration through gyroresonant wave particle interaction; and (iv) gamma-ray spectroscopy can provide new information on solar abundances, for example the site of the FIP-bias onset and the photospheric 3He abundance. We propose a new technique for the investigation of mass motion and mixing in the solar atmosphere: the observations of gamma-ray lines from long-term radioactivity produced by flare accelerated particles.

Type
Part I: Talks
Information
Symposium - International Astronomical Union , Volume 195: Highly Energetic Physical Processes and Mechanisms , 2000 , pp. 123 - 132
Copyright
Copyright © Astronomical Society of the Pacific 2000 

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