HR: 10:30h
AN: SP42A-01    [Abstracts]
TI: Energetics and Temporal Variability in RHESSI Gamma-Ray Flares
AU: * Shih, A Y
EM: ayshih@ssl.berkeley.edu
AF: Department of Physics and Space Sciences Laboratory, University of California, Berkeley, Berkeley, CA 94720 United States
AU: Smith, D M
EM: dsmith@scipp.ucsc.edu
AF: Department of Physics and Santa Cruz Institute for Particle Physics, University of California, Santa Cruz, Santa Cruz, CA 95064 United States
AU: Lin, R P
EM: rlin@ssl.berkeley.edu
AF: Department of Physics and Space Sciences Laboratory, University of California, Berkeley, Berkeley, CA 94720 United States
AU: Share, G H
EM: gerald.share@nrl.navy.mil
AF: E. O. Hulburt Center for Space Research, Naval Research Laboratory, Washington, DC 20375 United States
AU: Murphy, R J
EM: ronald.murphy@nrl.navy.mil
AF: E. O. Hulburt Center for Space Research, Naval Research Laboratory, Washington, DC 20375 United States
AU: Schwartz, R A
EM: richard.schwartz@gsfc.nasa.gov
AF: NASA Goddard Space Flight Center, Greenbelt Road, Greenbelt, MD 20771 United States
AU: Tolbert, A K
EM: kim.tolbert@gsfc.nasa.gov
AF: NASA Goddard Space Flight Center, Greenbelt Road, Greenbelt, MD 20771 United States
AB: The Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) has detected nuclear gamma-ray line emission from at least eleven solar flares over the past three years. These gamma-ray lines are produced when flare-accelerated ions collide with the ambient solar medium. In this paper, we concentrate on the energy content and time profiles of accelerated ions and electrons. Ion spectral information is derived from suitable line ratios. We also compare the fluxes and timing of gamma-ray emission and high-energy electron bremsstrahlung emission. Finally, for the larger flares, we investigate the temporal variability of the nuclear de-excitation lines as well.
DE: 7514 Energetic particles (2114)
DE: 7519 Flares
DE: 7554 X rays, gamma rays, and neutrinos
SC: Solar Physics Division - AAS [SP]
MN: 2005 Joint Assembly