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    Evolution of the Electron Distribution Function in the Whistler Wave Turbulence of the Solar Wind

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    Pierrard(2011b).pdf (696.2Kb)
    Authors
    Pierrard, V.
    Lazar, M.
    Schlickeiser, R.
    Discipline
    Physical sciences
    Audience
    Scientific
    Date
    2011
    Metadata
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    Description
    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
    uri: https://orfeo.belnet.be/handle/internal/3114
    doi: http://dx.doi.org/10.1007/s11207-010-9700-7
    scopus: 2-s2.0-79952696710
    Type
    Article
    Peer-Review
    Yes
    Language
    eng
    Links
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