Computer Science – Performance
Scientific paper
May 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsp42a..01l&link_type=abstract
American Geophysical Union, Spring Meeting 2008, abstract #SP42A-01
Computer Science
Performance
7519 Flares, 7526 Magnetic Reconnection (2723, 7835)
Scientific paper
Solar eruptions are sudden ejections of coronal plasma and magnetic field into the interplanetary medium, accompanied by large flares in the solar atmosphere. These events are the most dynamic phenomena in the solar corona and are important drivers of space weather through particle acceleration, flare-induced coronal heating, and the interaction of the ejecta with the Earth's magnetosphere. Magnetic reconnection is believed to be the key driver of these eruptions and their associated flares, and recently the combination of high resolution solar observations and high performance computing has allowed us to make breakthroughs in understanding how this reconnection proceeds. I will present simulations of the coronal reconnection and flaring which occur behind these eruptions, focusing on localized, three dimensional reconnection in a post-eruption current sheet. I will show how the resulting reconnected fields can form evacuated coronal downflows, hot arcades of post-eruption loops, and photospheric ribbons of H-alpha flare emission, as observed by solar missions such as SOHO, TRACE, STEREO and Hinode. I will then discuss the implications of this work for the creation of plasmoids via reconnection in the Earth's magnetotail current sheet.
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