Evolution of the Electron Distribution Function in the Whistler Wave Turbulence of the Solar Wind
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Authors
Pierrard, V.
Lazar, M.
Schlickeiser, R.
Discipline
Physical sciences
Audience
Scientific
Date
2011Metadata
Show full item recordDescription
The electron distribution functions from the solar corona to the solar wind are determined in this paper by considering the effects of the external forces, of Coulomb collisions and of the wave - particle resonant interactions in the plasma wave turbulence. The electrons are assumed to be interacting with right-handed polarized waves in the whistler regime. The acceleration of electrons in the solar wind seems to be mainly due to the electrostatic potential. Wave turbulence determines the electron pitch-angle diffusion and some characteristics of the velocity distribution function (VDF) such as suprathermal tails. The role of parallel whistlers can also be extended to small altitudes in the solar wind (the acceleration region of the outer corona), where they may explain the energization and the presence of suprathermal electrons.
Citation
Pierrard, V.; Lazar, M.; Schlickeiser, R. (2011). Evolution of the Electron Distribution Function in the Whistler Wave Turbulence of the Solar Wind. , Solar Physics, Vol. 269, Issue 2, 421-438, DOI: 10.1007/s11207-010-9700-7.Identifiers
scopus: 2-s2.0-79952696710
Type
Article
Peer-Review
Yes
Language
eng