HR: 1330h
AN: SH22A-0172    [PDF]
TI: Non-thermal Coronal Hard X-ray Emission Observed During a Partially Occulted Flare
AU: * Balciunaite, P
EM: balciunaite@ssl.berkeley.edu
AF: Space Sciences Lab, University of California, Berkeley, CA 94720-7450
AU: Krucker, S
EM: krucker@ssl.berkeley.edu
AF: Space Sciences Lab, University of California, Berkeley, CA 94720-7450
AU: Caspi, A
EM: cepheid@ssl.berkeley.edu
AF: Space Sciences Lab, University of California, Berkeley, CA 94720-7450
AU: Caspi, A
EM: cepheid@ssl.berkeley.edu
AF: Department of Physics, University of California, Berkeley, CA 94720
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: We will present an analysis of RHESSI hard X-ray imaging and spectroscopy of a GOES M1.5 class flare which occurred on 1 June 2003 0210-0700 UT in NOAA active region 0375 and was located 9 degrees behind the east limb of the Sun. Flare footpoints were thus occulted from view by ~9000 km, allowing for a relatively unobstructed detection of emission from the associated coronal sources. Throughout the duration of the flare, a thermal hard X-ray source can be seen rising with a velocity of ~7 km/s above GOES SXI soft X-ray and EIT ultraviolet (304A) loops. During the impulsive phase of the flare (0237-0310 UT), a non-thermal source is additionally seen above 15 keV with a relatively soft power law spectrum with an index around -5. This non-thermal source is displaced from the thermal source by up to 10,000 km and shows greater variations on a time scale of tens of seconds. We will present total energy estimates and a detailed analysis of the source motions during the flare. We will also discuss implications for models that postulate above-the-loop-top sources.
DE: 7509 Corona
DE: 7514 Energetic particles (2114)
DE: 7519 Flares
DE: 7524 Magnetic fields
DE: 7554 X rays, gamma rays, and neutrinos
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting