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    Electron velocity distribution functions from the solar wind to the corona

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    Authors
    Pierrard, V.
    Maksimovic, M.
    Lemaire, J.
    Discipline
    Physical sciences
    Audience
    Scientific
    Date
    1999
    Metadata
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    Description
    Typical electron velocity distribution functions observed at 1 AU from the Sun by the 3DP instrument onboard Wind are used as boundary conditions to determine the electron velocity distribution function at 4 solar radii in the corona. The velocity distribution functions (VDFs) at low altitude are obtained by solving the Fokker-Planck equation, using two different sets of boundary conditions. The first set typically corresponds to a VDF observed in a low-speed solar wind flow (i.e., characterized by "core" and "halo" electrons); the second one corresponds to high-speed solar wind (i.e., characterized by "core," "halo,", and "strahl" populations). We use the observed electron VDFs as test particles, which are submitted to external forces and Coulomb collisions with a background plasma. Closer to the Sun, the relative density of the core electrons is found to increase compared to the density of the halo population. Nevertheless, we find that in order to match the observed distributions at 1 AU, suprathermal tails have to be present in the VDF of the test electron at low altitudes in the corona.
    Citation
    Pierrard, V.; Maksimovic, M.; Lemaire, J. (1999). Electron velocity distribution functions from the solar wind to the corona. , Journal of Geophysical Research: Space Physics, Vol. 104, Issue A8, 17021-17032, , DOI: 10.1029/1999JA900169.
    Identifiers
    uri: https://orfeo.belnet.be/handle/internal/5345
    doi: http://dx.doi.org/10.1029/1999JA900169
    scopus: 2-s2.0-0000226554
    Type
    Article
    Peer-Review
    Yes
    Language
    eng
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