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    Coronal Temperature Profiles Obtained from Kinetic Models and from Coronal Brightness Measurements Obtained During Solar Eclipses

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    Pierrard(2014a).pdf (391.6Kb)
    Authors
    Pierrard, V.
    Borremans, K.
    Stegen, K.
    Lemaire, J.F.
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    Discipline
    Physical sciences
    Subject
    Corona
    Eclipse
    Heating
    Audience
    Scientific
    Date
    2014
    Metadata
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    Description
    Coronal density, temperature, and heat-flux distributions for the equatorial and polar corona have been deduced from Saito’s model of averaged coronal white-light (WL) brightness and polarization observations. These distributions are compared with those determined from a kinetic collisionless/exospheric model of the solar corona. This comparison indicates similar distributions at large radial distances (> 7 R⊙) in the collisionless region. However, rather important differences are found close to the Sun in the acceleration region of the solar wind. The exospheric heat flux is directed away from the Sun, while that inferred from all WL coronal observations is in the opposite direction, i.e. conducting heat from the inner corona toward the chromosphere. This could indicate that the source of coronal heating extends up into the inner corona, where it maximizes at r>1.5 R⊙, well above the transition region.
    Citation
    Pierrard, V.; Borremans, K.; Stegen, K.; Lemaire, J.F. (2014). Coronal Temperature Profiles Obtained from Kinetic Models and from Coronal Brightness Measurements Obtained During Solar Eclipses. , Solar Physics, Vol. 289, Issue 1, 183-192, DOI: 10.1007/s11207-013-0320-x.
    Identifiers
    uri: https://orfeo.belnet.be/handle/internal/2847
    doi: http://dx.doi.org/10.1007/s11207-013-0320-x
    scopus: 2-s2.0-84887950344
    Type
    Article
    Peer-Review
    Yes
    Language
    eng
    Links
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