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    Review of Solar Wind Entry into and Transport Within the Plasma Sheet

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    Wing(2014).pdf (6.856Mb)
    Authors
    Wing, S.
    Johnson, J.R.
    Chaston, C.C.
    Echim, M.
    Escoubet, C.P.
    Lavraud, B.
    Lemon, C.
    Nykyri, K.
    Otto, A.
    Raeder, J.
    Wang, C.-P.
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    Discipline
    Physical sciences
    Subject
    Double cusp (lobe) reconnection
    Entropy
    Fast flow
    Ion outflow
    Ion to electron temperature ratio
    Kelvin-Helmholtz
    Kinetic Alfvén wave (KAW)
    Particle transport
    Solar wind entry
    Turbulence
    Audience
    Scientific
    Date
    2014
    Metadata
    Show full item record
    Description
    The plasma sheet is populated in part by the solar wind plasma. Four solar entry mechanisms are examined: (1) double cusp or double lobe reconnection, (2) Kelvin-Helmholtz Instability (KHI), (3) Kinetic Alfvén waves (KAW), and (4) Impulsive Penetration. These mechanisms can efficiently fill the plasma sheet with cold dense ions during northward interplanetary magnetic field (IMF). The solar wind ions appear to have been heated upon entry along the plasma sheet dawn flank. The cold-component (solar wind origin) ion density is higher on the dawn flank than the dusk flank. The asymmetric evolution of the KAW and magnetic reconnection in association with the KHI at the dawn and dusk flank magnetopause may partly produce the dawn-dusk temperature and density asymmetries. Solar wind that crosses the magnetopause lowers the specific entropy (s=p/ρ γ ) of the plasma sheet along the flanks. Subsequent transport of the cold ions from the flanks to the midnight meridian increases s by a factor of 5. T i , T e , s i , and s e increase when the solar wind particles are transported across the magnetopause, but T i /T e is roughly conserved. Within the magnetotail, E×B and curvature and gradient drifts play important roles in the plasma transport and can explain the large features seen in the plasma sheet. Turbulence can also play a significant role, particularly in the cold plasma transport from the flanks to the midnight meridian. Total entropy (S=pV γ ) conservation provides important constraints on the plasma sheet transport, e.g., fast flows.
    Citation
    Wing, S.; Johnson, J.R.; Chaston, C.C.; Echim, M.; Escoubet, C.P.; Lavraud, B.; Lemon, C.; Nykyri, K.; Otto, A.; Raeder, J.; Wang, C.-P. (2014). Review of Solar Wind Entry into and Transport Within the Plasma Sheet. , Space Science Reviews, Vol. 184, Issue 1-4, 33-86, DOI: 10.1007/s11214-014-0108-9.
    Identifiers
    uri: https://orfeo.belnet.be/handle/internal/2833
    doi: http://dx.doi.org/10.1007/s11214-014-0108-9
    scopus: 2-s2.0-84911977864
    Type
    Article
    Peer-Review
    Yes
    Language
    eng
    Links
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