Stochastic acceleration of solar flare protons

Details Stochastic acceleration of solar flare protons Stochastic acceleration of solar flare protons

Oct 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...233..383b&link_type=abstract

Astrophysical Journal, Part 1, vol. 233, Oct. 1, 1979, p. 383-394.

Mathematics

Logic

53

Magnetohydrodynamic Waves, Particle Acceleration, Solar Flares, Solar Protons, Boundary Value Problems, Diffusion Coefficient, Magnetohydrodynamics, Mathematical Models, Nucleons, Transit Time

Scientific paper

The acceleration of solar flare protons by the cyclotron damping of intense Alfven wave turbulence in a magnetic trap is considered. The energy diffusion coefficient is computed for a near-isotropic distribution of super-Alfvenic protons, and a steady-state solution for the particle spectrum is found for both transit-time and diffusive losses out of the ends of the trap. The acceleration time to a characteristic energy of about 20 MeV per nucleon can be as short as 10 sec. On the basis of phenomenological arguments, it is inferred that the Alfven wave spectrum typically has an inverse square frequency dependence and that the correlation time of the turbulence lies in the range between 0.5 and 50 msec.

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