HR: 1330h
AN: SH53A-02    [Abstracts]
TI: Active region evolution in the build-up to large solar energetic particle events
AU: * Alexander, D
EM: dalex@rice.edu
AF: Rice University, Dept. Physics and Astronomy MS-108 6100 Main St, Houston, TX 77005 United States
AU: Coyner, A
EM: acoyner@rice.edu
AF: Rice University, Dept. Physics and Astronomy MS-108 6100 Main St, Houston, TX 77005 United States
AU: Daou, A
EM: agdaou@rice.edu
AF: Rice University, Dept. Physics and Astronomy MS-108 6100 Main St, Houston, TX 77005 United States
AU: Liu, R
EM: rliu@rice.edu
AF: Rice University, Dept. Physics and Astronomy MS-108 6100 Main St, Houston, TX 77005 United States
AB: The SEP signatures of the solar flares occurring on 21 Apr 2002 and 24 Aug 2002 show marked differences in their compositions above 10 MeV/nucleon, yet at the Sun the events themselves display very similar characteristics in the chromospheric (hard X-ray) emission and their coronal (X-ray, EUV) signatures. We consider the prior evolution of the parent active regions to look for possible signatures in the ambient corona, magnetic connectivities (within the active region, large-scale closed field, and open field distributions), and flare/activity history which may differentiate the solar conditions leading to the observed disparate particle signatures at 1 AU.
DE: 7509 Corona
DE: 7513 Coronal mass ejections
DE: 7519 Flares
DE: 7524 Magnetic fields
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2005 Joint Assembly