Non-stochastic prompt proton acceleration by fast magnetosonic shocks in the solar plasma

Theoretical and numerical analyses are carried out for plasma heating and proton acceleration (V x B) due to magnetosonic shock waves (MSW) in the solar plasma. A simple model is developed for V x B acceleration by examining a single-particle orbit in a high-amplitude monochromatic electrostatic wave moving in a direction perpendicular to an external magnetic field. The particle can attain the E x B drift velocity. The model is used to derive the maximum velocity a particle can attain when driven by quasi-parallel and quasi-perpendicular MSW. Acceleration is found to be significantly stronger witn the latter, as is demonstrated with results of a 2.5 dimension simulation of acceleration by a quasi-perpendicular MSW. Implications of the results for modeling coronal heating and proton acceleration by MSWs produced by solar flares are discussed. 39 references.