HR: 11:45h
AN: SP52A-06    [Abstracts]
TI: Coronal X-ray Emission in Long-Duration Occulted Flares
AU: * Balciunaite, P
EM: balciunaite@ssl.berkeley.edu
AF: Space Sciences Lab, University of California, Berkeley, CA 94720-7450
AU: Christe, S D
EM: schriste@ssl.berkeley.edu
AF: Space Sciences Lab, University of California, Berkeley, CA 94720-7450
AU: Christe, S D
EM: schriste@ssl.berkeley.edu
AF: Department of Physics, University of California, Berkeley, CA 94720
AU: Krucker, S
EM: krucker@ssl.berkeley.edu
AF: Space Sciences Lab, University of California, Berkeley, CA 94720-7450
AU: Lin, R P
EM: rlin@ssl.berkeley.edu
AF: Space Sciences Lab, University of California, Berkeley, CA 94720-7450
AU: Lin, R P
EM: rlin@ssl.berkeley.edu
AF: Department of Physics, University of California, Berkeley, CA 94720
AB: To investigate coronal X-ray (≥ 6 keV) emission using RHESSI, we select long-duration (≥ 3 h) flares with completely or partially occulted footpoints. Flare footpoint sources dominate and thus obstruct the observation of coronal emission; short durations do not allow enough time for observation of various changes. We examine the location, morphology, size, height, and spectral characteristics in 20 long-duration flares seen with RHESSI whose footpoints are occulted by the solar limb to at most 30°. In 4 cases we see hard X-ray (≥ 20 keV) coronal sources; in the remaining cases hard X-ray emission comes from partially occulted footpoints only or the coronal emission is thermal.
DE: 7509 Corona
DE: 7519 Flares
SC: Solar Physics Division - AAS [SP]
MN: 2005 Joint Assembly