Solar coronal heating by plasma waves

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Bingham, R. and Shukla, P.K. and Eliasson, Bengt and Stenflo, L. (2010) Solar coronal heating by plasma waves. Journal of Plasma Physics, 76 (2). pp. 135-158. ISSN 0022-3778 (http://dx.doi.org/10.1017/S0022377809990031)

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Abstract

The solar coronal plasma is maintained at temperatures of millions of degrees, much hotter than the photosphere, which is at a temperature of just 6000 K. In this paper, the plasma particle heating based on the kinetic theory of wave-particle interactions involving kinetic Alfvén waves and lower-hybrid drift modes is presented. The solar coronal plasma is collisionless and therefore the heating must rely on turbulent wave heating models, such as lower-hybrid drift models at reconnection sites or the kinetic Alfvén waves. These turbulent wave modes are created by a variety of instabilities driven from below. The transition region at altitudes of about 2000 km is an important boundary chromosphere, since it separates the collision-dominated photosphere/chromosphere and the collisionless corona. The collisionless plasma of the corona is ideal for supporting kinetic wave-plasma interactions. Wave-particle interactions lead to anisotropic non-Maxwellian plasma distribution functions, which may be investigated by using spectral analysis procedures being developed at the present time.

ORCID iDs

Bingham, R. ORCID logoORCID: https://orcid.org/0000-0002-9843-7635, Shukla, P.K., Eliasson, Bengt ORCID logoORCID: https://orcid.org/0000-0001-6039-1574 and Stenflo, L.;
  • Item type:Article
    ID code:27169
    Dates:
    Date
    Event
    April 2010
    Published
    Subjects:Science > Physics
    Department:Faculty of Science > Physics
    Depositing user:Users 1261 not found.
    Date deposited:30 Aug 2010 08:34
    Last modified:11 Nov 2024 09:36
    Related URLs:
    URI:https://strathprints.strath.ac.uk/id/eprint/27169
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