Plasma Heating Due to Spectrum of Obliquely Propagating Alfven Waves

Details Plasma Heating Due to Spectrum of Obliquely Propagating Alfven Waves Plasma Heating Due to Spectrum of Obliquely Propagating Alfven Waves

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsh12a0402d&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #SH12A-0402

Physics

2118 Energetic Particles, Solar, 2149 Mhd Waves And Turbulence, 7807 Charged Particle Motion And Acceleration, 7839 Nonlinear Phenomena, 7867 Wave/Particle Interactions

Scientific paper

It has been shown recently that, contrary to conventional analysis, significant perpendicular heating of a magnetized plasma can be effected by waves with frequencies well below the ion cyclotron frequency. It was preliminarily shown that a perturbation consisting of a spectrum of modes results in an increased heating efficiency as compared with a single mode. Motivated by this result, we have undertaken a detailed study of the dependence of the heating efficiency, due to a spectrum of obliquely propagating Alfven waves, on the wave energy density, spectral indices, and perpendicular wave scales. We have simulated the interaction of an initially cold plasma with the low and high frequency halves(with respect to the cyclotron frequency) of a given wave spectrum, acting both independently and in unison. It is found that a spectrum including only modes below the cyclotron frequency could indeed impart significant heating, while the higher frequency modes remain most efficient. In addition, it is found that the perpendicular wave scale, which allows for the nonlinear cyclotron resonance, also limits the attainable particle perpendicular energy, due to the finite Larmor-radius averaging effect. This work serves as a promising model for heating of the solar corona as it does not rely on the primary cyclotron resonance. Both analytical and numerical detailed results will be presented. Work supported in part by US DOE, NSF and UCI UROP grants.

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