[65.08] MHD Modeling of CMEs near the Sun

AAS 200th meeting, Albuquerque, NM, June 2002
Session 65. The Magnetic Structure of CMEs
SPD Topical Session Oral, Wednesday, June 5, 2002, 2:30-4:00pm, 4:15-6:00pm, Ruidoso/Pecos

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[65.08] MHD Modeling of CMEs near the Sun

P. Riley, Z. Mikic, J. A. Linker, R. Lionello (SAIC)

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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