Astronomy and Astrophysics – Astrophysics
Scientific paper
Mar 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...406..298s&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 406, no. 1, p. 298-305.
Astronomy and Astrophysics
Astrophysics
5
Magnetohydrodynamic Turbulence, Magnetohydrodynamic Waves, Particle Acceleration, Solar Corona, Solar Protons, Solar Flares, Wave Propagation
Scientific paper
We consider coronal proton acceleration by a spectrum of MHD waves in the geometry of a magnetic loop including wave-wave interactions. The dominant wave-wave interaction is scattering on the polarization clouds of ions, which leads to the transformation of Alfven waves among themselves and with fast magnetosonic waves, and the transformation of fast magnetosonic waves among themselves. These processes can have a large indirect effect on the acceleration process because the thermal protons are heated or accelerated by beat-wave processes, allowing many more protons to satisfy the injection condition for acceleration. As a result, assuming that the source of turbulence has a limited energy reserve, the turbulence energy is 'burned out' in proton acceleration on a time scale of a few to several seconds, depending on the exact conditions. The plausibility of this scenario is demonstrated.
Brecht Stephen H.
Smith Donelson F.
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