Kinetic Processes in Solar Physics

Details Kinetic Processes in Solar Physics Kinetic Processes in Solar Physics

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008espm...12..1.3m&link_type=abstract

"12th European Solar Physics Meeting, Freiburg, Germany, held September, 8-12, 2008. Online at http://espm.kis.uni-freiburg.de/,

Physics

Scientific paper

Non-maxwellian particle distributions seem to occur commonly in the collisionless conditions of the corona and solar wind. The most extreme examples accompany the events of solar flares, when we find ions on occasions attaining energies in the 10 GeV range. In the denser atmosphere, temperature scale lengths comparable to mean free paths will induce strongly non-maxwellian distributions. Even when there is no direct evidence for their presence, we must expect these to be present in low density plasmas.
How do we account for these distributions? What roles must they play in energy transport, in equilibrium and stability, in the interpretation of diagnostics? We first review some textbook ideas on the situations that demand kinetic descriptions, and the extent to which this can be achieved via moment descriptions. We next consider some key problems in solar physics: thermal conductivity in steep temperature gradients; energy release and particle acceleration in solar flares; the origin of non-maxwellian velocity distributions in the solar wind; coherent radio emission. In each case we try to characterise the problem in a general way, then discuss some recent advances in understanding.
We conclude with some comments on the implications of such distributions in situations where their presence is at first not recognised.

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