HR: 09:00h
AN: SH41A-04    [PDF]
TI: Eruptive Behavior Originating in Active Regions
AU: * Linker, J A
EM: linkerj@saic.com
AF: SAIC, 10260 Campus Point Drive, San Diego, CA 92121
AU: Mikic, Z
EM: mikicz@saic.om
AF: SAIC, 10260 Campus Point Drive, San Diego, CA 92121
AU: Lionello, R
EM: lionellor@saic.com
AF: SAIC, 10260 Campus Point Drive, San Diego, CA 92121
AU: Riley, P
EM: pete.riley@saic.com
AF: SAIC, 10260 Campus Point Drive, San Diego, CA 92121
AU: Amari, T
EM: amari@cpht.polytechnique.fr
AF: Centre de Physique Theorique, Ecole Polytechnique, Palaiseau Cedex, 91128 France
AB: Coronal mass ejections (CMEs) are spectacular manifestations of solar acitivy. These immense eruptions of plasma and magnetic field are propelled outward from the sun with velocities as high as 2000 km/s. The fastest CMEs typically originate from active regions on the Sun. MHD models of the eruption of large scale coronal fields have demonstrated significant energy release in idealized 2D (Antiochos et al., ApJ 512, 985, 1999) and 3D (Linker et al., Phys. Plasmas 10, 1971, 2003) geometry. Eruptive behavior has also been shown for a 3D localized arcade (Amari et al., ApJ 529, L49, 2000). In active regions on the Sun, both the localized field due to the active region and the overlying fields in the large scale corona are important. We describe MHD computations of the eruptive behavior of a localized active region field (modeled as a localized bipole) within a large-scale dipolar configuration. We discuss the differences between this more realistic configuration and the idealized configurations that have been considered previously. 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: 2003 Fall Meeting