On the Cascading Acceleration of the Quasi-Thermal Electrons by mhd Turbulence in Solar Flares

Details On the Cascading Acceleration of the Quasi-Thermal Electrons by mhd Turbulence in Solar Flares On the Cascading Acceleration of the Quasi-Thermal Electrons by mhd Turbulence in Solar Flares

May 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000soph..194..131t&link_type=abstract

Solar Physics, v. 194, Issue 1, p. 131-136 (2000).

Physics

10

Scientific paper

A model of the cascading acceleration of quasi-thermal electrons by MHD turbulence in solar flares is considered. Analysis shows that fast magnetoacoustic wave modes with large wavenumbers (>3×10^-8 cm^-1) strongly damp due to ion viscosity for both preflare and flare conditions. The viscous damping of fast magnetoacoustic wave modes is 10-100 times more efficient than Fermi or transit-time electron acceleration.

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