Turbulent acceleration of superthermal electrons

Details Turbulent acceleration of superthermal electrons Turbulent acceleration of superthermal electrons

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsm53b1284r&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SM53B-1284

Physics

7845 Particle Acceleration

Scientific paper

The acceleration and heating of charged particles in the solar wind is one of the outstanding problems in contemporary solar and heliospheric physics. Electron distributions with various degrees of asymmetry associated with the energetic tail population are commonly detected in the solar wind near 1 AU. Traditional attempt to address the origin of superthermal electrons usually starts from the collisional dynamics near the Sun and their transport through interplanetary space. In the present paper, we look for collective mechanism(s) as an alternative explanation for the generation of superthermal population. By numerically solving one-dimensional electrostatic weak turbulence equations and by performing fully nonlinear particle-in-cell (PIC) simulations, this paper demonstrates that a wide variety of asymmetric energetic tail distribution may result. It is found that a wide variety of asymmetric tail formation becomes possible if one posits that the solar wind electrons are initially composed of thermal core plus field-aligned counter-streaming beams, instead of the customary thermal population plus a single beam. It is shown that the resulting nonlinear wave-wave and wave-particle interactions lead to asymmetric non-thermal tails.

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