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The Relation Between Escape and Scattering Times of Energetic Particles in a Turbulent Magnetized Plasma: Application to Solar Flares View all abstracts by submitter

Vahe Patrosian   Submitted: 2018-08-24 13:43

The relation between time scales of particle escape from and scattering in the acceleration regions of many space and astrophysical sources is of critical importance in the analysis of emission signatures produced by these particles and in the determination of the acceleration and transport mechanisms at work. This paper addresses this general problem, in particular in solar flares, where in addition to scattering by turbulence, the magnetic field convergence from the acceleration region towards the boundaries of the acceleration region also influences the particle escape. We test an analytical approximation of this relation with a numerical model of particle transport. To this end, a kinetic Fokker-Planck transport model of particles is solved with a stochastic differential equation scheme. This approach enables further insights into the phase-space dynamics of the transport process, which would otherwise not be accessible. We find that in general the numerical results agree well with the approximate analytic equation, however, there are also significant differences due to the initial pitch-angle distribution in a weak scattering regime. The results are important in the interpretation of observations of energetic particles in solar flares and other similar space and astrophysical acceleration sites, and for the determination of acceleration-transport coefficients, commonly used in Fokker-Planck type kinetic equations

Authors: Frederic Effenberger and Vahé Petrosian
Projects: None

Publication Status: Submitted to Astrophysical Journal
Last Modified: 2018-08-27 11:22
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