The propagation of solar flare particles in a turbulent coronal loop

Details The propagation of solar flare particles in a turbulent coronal loop The propagation of solar flare particles in a turbulent coronal loop

Aug 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985icrc....4....1r&link_type=abstract

In NASA. Goddard Space Flight Center 19th Intern. Cosmic Ray Conf., Vol. 4 p 1 (SEE N85-34729 23-92)

Computer Science

Coronal Loops, Electron Scattering, Electrons, Plasma Turbulence, Proton Scattering, Solar Flares, Solar Protons, Chromosphere, Diffusion Coefficient, Energy Dissipation, Gamma Ray Bursts, Particle Acceleration, Time Dependence, X Rays

Scientific paper

Energetic solar flare particles, both electrons and protons, must survive the turbulent environment of a flaring loop and propogate to the lower corona or chromosphere in order to produce hard X-ray and gamma ray bursts. This plasma turbulence, often observed in soft X-ray line widths to be in excess of 100 km/s, is presumably capable of efficiently scattering the fast flare particles. This prevents to some degree the free streaming of accelerated particles and depending on the amplitude of the turbulence, restricts the particles to diffusive propagation along the length of the loop to the target chromosphere. In addition this turbulence is capable of performing additional acceleration of the fast particles by the second order Fermi mechanism. For compact flares with rise times 10s, the acceleration effect is small and the propagation of the particles is governed by spatial diffusion and energy loss in the ambient medium. The solution of the time dependent diffusion equation with velocity dependent diffusion and energy loss coefficients yields for the case of nonrelativistic protons particle precipitation rates which are necessary for calculating thick target gamma ray emission and also yields the total thin target emissivity.

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