MHD Modeling of CMEs near the Sun

Details MHD Modeling of CMEs near the Sun MHD Modeling of CMEs near the Sun

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...200.6508r&link_type=abstract

American Astronomical Society, 200th AAS Meeting, #65.08; Bulletin of the American Astronomical Society, Vol. 34, p.752

Astronomy and Astrophysics

Astronomy

Scientific paper

Coronal Mass Ejections (CMEs) are spectacular events involving the expulsion of significant amounts of solar material and energy into the heliosphere. In spite of their importance, the physical mechanisms leading to their eruption are not well known. In this talk, we review how the magnetohydrodynamic (MHD) fluid description is applied to model the initiation and evolution of CMEs near the Sun. In particular, we describe: how the ambient solar corona is first established; how energy is stored in the corona prior to eruption; and how either magnetic shear and/or flux cancellation can subsequently lead to the eruption of magnetic flux ropes with different physical properties. Research supported by NASA and NSF.

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