Abstract
Gamma-ray emission from solar flares is generally beleived to be produced by nuclear reactions between energetic ions and ambient material in the lower solar atmosphere. We consider the propagation of flare accelerated ions from the corona to the lower atmosphere, taking into account the mirror force on the particles due to the increase of the magnetic field strength with depth. We show that for reasonable models of the magnetic field structure, the mirror force constrains all but a narrow loss cone of particles from penetrating promptly to the lower atmosphere. This has observation consequences for the intensity and time profile of the ..gamma..-ray emission, and it could affect inferences about the timing and nature of the acceleration mechanism of flare accelerated particles.
Published Version
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