Generation of Electron Suprathermal Tails in the Upper Solar Atmosphere: Implications for Coronal Heating

Details Generation of Electron Suprathermal Tails in the Upper Solar Atmosphere: Implications for Coronal Heating Generation of Electron Suprathermal Tails in the Upper Solar Atmosphere: Implications for Coronal Heating

Jan 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000apj...528..509v&link_type=abstract

The Astrophysical Journal, Volume 528, Issue 1, pp. 509-523.

Astronomy and Astrophysics

Astronomy

38

Acceleration Of Particles, Plasmas, Sun: Chromosphere, Sun: Corona, Waves

Scientific paper

We present a mechanism for the generation of non-Maxwellian electron distribution function in the upper regions of the solar atmosphere in the presence of collisional damping. It is suggested that finite-amplitude, low-frequency, obliquely propagating electromagnetic waves can carry a substantial electric field component parallel to the mean magnetic field that can be significantly larger than the Dreicer electric field. This long-wavelength electric fluctuation is capable of generating high-frequency electron plasma oscillations and low-frequency ion acoustic-like waves. The analysis has been performed using 1-1/2D Vlasov and PIC numerical simulations in which both electrons and ions are treated kinetically and self consistently. The simulation results indicate that high-frequency electron plasma oscillations and low-frequency ion acoustic-like waves are generated. The high-frequency electron plasma oscillation drives electron plasma turbulence, which subsequently is damped out by the background electrons. The turbulence damping results in electron acceleration and the generation of non-Maxwellian suprathermal tails on timescales short compared to collisional damping. Bulk heating also occurs if the fluctuating parallel electric field is strong enough. This study suggests that finite-amplitude, low-frequency, obliquely propagating electromagnetic waves can play a significant role in the acceleration and heating of the solar corona electrons and in the coupling of medium and small-scale phenomena.

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