About the prominence heating mechanisms during its eruptive phase

Details About the prominence heating mechanisms during its eruptive phase About the prominence heating mechanisms during its eruptive phase

Aug 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002soph..208..283f&link_type=abstract

Solar Physics, v. 208, Issue 2, p. 283-295 (2002).

Physics

26

Scientific paper

Recent EUV observations reveal that the `image' of the prominence overlaying coronal emission sometimes suddenly changes from absorption of EUV radiation to emission during the eruptive phase. This change reveals fast heating of the plasma within the prominence. We propose a kinetic mechanism of heating the fluid particles that transforms magnetic energy of the pre-eruptive magnetic configuration stored in the filament electric current into heat through collision processes of counteracting flows. The shape of the flux that the filament is made of should include upward concave segments to provide the counter flows within the erupting prominence. A typical twisted flux rope easily meets this requirement. Gas dynamic calculations are offered in addition to permit a quantitative evaluation of the relevant parameters and their time variations.

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