Magnetic Reconnection in Solar Flares and Coronal Mass Ejections

Details Magnetic Reconnection in Solar Flares and Coronal Mass Ejections Magnetic Reconnection in Solar Flares and Coronal Mass Ejections

Apr 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aps..aprk12003a&link_type=abstract

American Physical Society, April Meeting, Jointly Sponsored with the High Energy Astrophysics Division (HEAD) of the American As

Astronomy and Astrophysics

Astrophysics

Scientific paper

Magnetic reconnection is, perhaps, the most important process in space plasmas for transferring energy from magnetic fields to matter. In particular, reconnection is believed to be the underlying driver of the giant explosive releases of magnetic energy in the Sun's atmosphere that are observed as a solar flare and/or coronal mass ejection (CME) event. First, I will present compelling evidence for reconnection in flares and CMEs from the spectacular observations by TRACE and SOHO. Next the recent advances in reconnection theory will be reviewed, and their implications for flare/cme models will be discussed. Simulations will be presented of the recently developed "breakout" model for eruptive flares/CMEs, in which reconnection plays the key role in initiating the event. This work was supported in part by NASA and ONR.

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