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Solar coronal heating by plasma waves

Published online by Cambridge University Press:  16 June 2009

R. BINGHAM,
P. K. SHUKLA,
B. ELIASSON and
L. STENFLO
R. BINGHAM
Affiliation:
Rutherford Appleton Laboratory, Chilton, Oxon, OX11 0QX, UK (bob.bingham@stfc.ac.uk, ps@tp4.ruhr-uni-bochum.de)
P. K. SHUKLA
Affiliation:
Institut für Theoretische Physik IV, Ruhr-Universität Bochum, D-44780 Bochum, Germany
B. ELIASSON
Affiliation:
Department of Physics, Umeå University, SE-90187 Umeå, Sweden
L. STENFLO
Affiliation:
Department of Physics, Umeå University, SE-90187 Umeå, Sweden
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Abstract

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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.

Information

Type
Papers
Information
Journal of Plasma Physics , Volume 76 , Issue 2 , April 2010, pp. 135 - 158
Copyright
Copyright © Cambridge University Press 2009

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