Physics
Scientific paper
May 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsp31d..05l&link_type=abstract
American Geophysical Union, Spring Meeting 2008, abstract #SP31D-05
Physics
7509 Corona, 7513 Coronal Mass Ejections (2101), 7524 Magnetic Fields, 7531 Prominence Eruptions
Scientific paper
Since the first observations of EIT waves in the May 1997 CME event (Thompson et al. 1998), their origin and nature has been the subject of considerable debate. Explanation for the signatures include a fast mode shock (Uchida, 1968), fast mode waves (Wang 2000, Wu et al. 2001, Ofman & Thompson 2002, Warmuth et al. 2004, Ofman 2007), solitons (Wills-Davey et al. 2007), and opening of the magnetic field associated with the erupting CME (Attril et al. 2007, Delannee et al. 2008). We have developed MHD models that include energy transport (radiative losses, anisotropic thermal conduction, and coronal heating) in the transition region and solar corona. This more accurate representation of energy flow allows us to compute simulated EUV and X-ray emission and compare directly with observations. We have developed an MHD simulation of the May 97 event, with many characteristics of the actual event, including waves that appear in simulated EIT images. We discuss the analysis of these waves in relation to popular hypotheses for EIT waves. Work supported by NASA and CISM, an NSF Science and Technology Center.
Linker Jon A.
Lionello Roberto
Mikic Zoran
Riley Pete
Titov Vasily V.
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