HR: 16:30h
AN: SH54B-05    [Abstracts]
TI: Modeling Active Region Coronal Mass Ejections*
AU: * Linker, J A
EM: linkerj@saic.com
AF: Science Applications International Corporation, 10260 Campus Point Drive, San Diego, CA 92121-1578
AU: Mikic, Z
EM: mikicz@saic.com
AF: Science Applications International Corporation, 10260 Campus Point Drive, San Diego, CA 92121-1578
AU: Titov, V
EM: viacheslav.s.titov@saic.com
AF: Science Applications International Corporation, 10260 Campus Point Drive, San Diego, CA 92121-1578
AU: Lionello, R
EM: lionellor@saic.com
AF: Science Applications International Corporation, 10260 Campus Point Drive, San Diego, CA 92121-1578
AU: Riley, P
EM: pete.riley@saic.com
AF: Science Applications International Corporation, 10260 Campus Point Drive, San Diego, CA 92121-1578
AB: The fastest coronal mass ejections (CMEs) typically originate from active regions on the Sun. From a theoretical standpoint, fast CMEs are the most difficult to understand and model, because they require that large amounts of magnetic energy (10³² ergs) be released rapidly (~1000 seconds). We describe MHD computations of eruptive behavior in an active region arising from the flux cancellation mechanism. The active region is modeled as a localized bipole within a global dipolar configuration, and is similar to the solar magnetic flux for the May 12, 1997 CME. We find that a localized 3D configuration erupts as a consequence of flux cancellation, in the same way that 2D axisymmetric and large-scale 3D fields erupt. We discuss the role of the interaction of the local active region magnetic field with the global magnetic fields due to the surrounding magnetic flux, as well the implications of our work for the initiation of fast CMEs. *Work supported by NASA and the Center for Integrated Space Weather Modeling (an NSF Science and Technology Center).
DE: 7509 Corona
DE: 7513 Coronal mass ejections
DE: 7524 Magnetic fields
DE: 7531 Prominence eruptions
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2005 Joint Assembly