Candidate coronal mass ejection heating mechanisms

Details Candidate coronal mass ejection heating mechanisms Candidate coronal mass ejection heating mechanisms

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh23b1836m&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH23B-1836

Astronomy and Astrophysics

Astrophysics

[7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7526] Solar Physics, Astrophysics, And Astronomy / Magnetic Reconnection, [7549] Solar Physics, Astrophysics, And Astronomy / Ultraviolet Emissions

Scientific paper

Several recent observational results suggest that coronal mass ejection (CME) plasma is heated even after leaving the flare site. The source of the heating is probably the magnetic field, but the mechanisms that convert magnetic to thermal energy during these events are not well understood. In the context of CMEs observed by SOHO/UVCS and analyzed using a time-dependent ionization code, we assess the efficacy of several candidate mechanisms, including heating by the CME current sheet, kink/tearing instabilities of the flux rope, turbulence, thermal conduction, energetic particles, and wave heating. Further tests of these models require investigating many events using a standardized method, so we discuss progress on automating this time-dependent ionization technique to constrain heating rates for a large number of CMEs.

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