HR: 1340h
AN: SH23A-0313    [Abstracts]
TI: Gamma-ray Imaging of the 2005 January 20 Solar Flare
AU: * Hurford, G J
EM: ghurford@ssl.berkeley.edu
AF: Space Sciences Lab, University of California, Berkeley, CA 94720 United States
AU: Krucker, S
EM: krucker@ssl.berkeley.edu
AF: Space Sciences Lab, University of California, Berkeley, CA 94720 United States
AU: Lin, R P
EM: boblin@ssl.berkeley.edu
AF: Space Sciences Lab, University of California, Berkeley, CA 94720 United States
AU: Schwartz, R A
EM: richard.schwartz@gsfc.nasa.gov
AF: NASA/GSFC and SSAI, n/a, Greenbelt, MD 20771 United States
AU: Smith, D M
EM: dsmith@scipp.ucsc.edu
AF: Dept of Physics, Santa Cruz Institute for Particle Physics, University of California, Santa Cruz, CA 95064 United States
AB: Solar gamma-ray emission provides the only available observational perspective on flare-accelerated ions near the Sun. Inelastic collisions between accelerated ions and the ambient solar atmosphere produces prompt line emission, a Doppler-broadened gamma-ray continuum as well as narrow lines due to positron annihilation (511 keV) and neutron capture (2.2 MeV). In addition to this ion-related emission, there is a significant electron-bremsstrahlung contribution from electrons accelerated to energies up to 10 MeV and beyond. The 2002 January 20 event provided one of the hardest ion and electron spectra observed to date. In this paper, we report on the results of gamma-ray imaging from ~100 keV through 7 MeV, including the gamma-ray continuum and neutron-capture line. Emphasis will be on the spatial distribution of the emission as a function of energy.
DE: 7514 Energetic particles (2114)
DE: 7519 Flares
DE: 7554 X-rays, gamma rays, and neutrinos
SC: SPA-Solar and Heliospheric Physics [SH]
MN: Fall Meeting 2005