HR: 08:30h
AN: SH31A-03    [Abstracts]
TI: Hard X-ray Emission From Coronal Electron Beams Associated With Type III Radio Bursts
AU: * Saint-Hilaire, P
EM: shilaire@ssl.berkeley.edu
AF: Space Sciences Laboratory, 7 Gauss Way, Berkeley, CA 94720 United States
AU: Krucker, S
EM: krucker@ssl.berkeley.edu
AF: Space Sciences Laboratory, 7 Gauss Way, Berkeley, CA 94720 United States
AU: Lin, R P
EM: rlin@ssl.berkeley.edu
AF: Space Sciences Laboratory, 7 Gauss Way, Berkeley, CA 94720 United States
AB: For the first time, a concerted effort to find X-ray emission from Type III-generating electron beams propagating in the solar corona has been undertaken. Spatially-integrated and imaging spectroscopy of partial thick-target hard X-ray bremsstrahlung emission from electron beams propagating outwards in the solar corona have been numerically modeled, and folded through the RHESSI (and GOES) instrumental response. The extensive RHESSI simulation software has been used to evaluate the possibility of detection of such X-rays. Under the assumption that Type III radio bursts are produced by the same kind of electron beams that generate the usually-observed flare hard X-rays (in our case, we are interested in beams going outwards rather than precipitating in the chromosphere), it is clear that they should be observable in X-rays with RHESSI, at least when the flare is occulted (footpoints behind the solar limb). I will present and discuss observations made with RHESSI and radio observatories.
DE: 7509 Corona
DE: 7514 Energetic particles (2114)
DE: 7534 Radio emissions
DE: 7554 X-rays, gamma rays, and neutrinos
SC: SPA-Solar and Heliospheric Physics [SH]
MN: Fall Meeting 2005