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    A transonic collisionless model of the solar wind

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    Zouganelis(2004a).pdf (342.8Kb)
    Authors
    Zouganelis, I.
    Maksimovic, M.
    Meyer-Vernet, N.
    Lamy, H.
    Issautier, K.
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    Discipline
    Physical sciences
    Audience
    Scientific
    Date
    2004
    Metadata
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    Description
    Because of the seraicollisional nature of the solar wind, the collisionless or exospheric approach and the hydrodynamic one are both inaccurate. However, the advantage of simplicity makes them useful for enlightening us on some basic mechanisms of solar wind acceleration. Previous exospheric models have been able to reproduce winds that were already nearly supersonic at the exobase, the altitude above which there are no collisions. In order to allow transonic solutions, a lower exobase has to be considered, in which case the protons are experiencing a nonmonotonic potential energy profile. This is done in the present work. In this model, the electron velocity distribution in the corona is assumed to be nonthermal. Parametric results are presented and show that the high acceleration obtained does not depend on the details of the nonthermal distributions. This acceleration seems, therefore, to be a robust result produced by the presence of a sufficient number of suprathermal electrons. A method for improving the exospheric description is also given, which consists of mapping particle orbits in terms of their invariants of motion.
    Citation
    Zouganelis, I.; Maksimovic, M.; Meyer-Vernet, N.; Lamy, H.; Issautier, K. (2004). A transonic collisionless model of the solar wind. , Astrophysical Journal, Vol. 606, Issue 1, 542-554, DOI: 10.1086/382866.
    Identifiers
    uri: https://orfeo.belnet.be/handle/internal/5091
    doi: http://dx.doi.org/10.1086/382866
    scopus: 2-s2.0-2542536214
    Type
    Article
    Peer-Review
    Yes
    Language
    eng
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