HR: 13:45h
AN: SH33A-02    [Abstracts]
TI: Relationship of Solar Flare Accelerated Particles to Solar Energetic Particles (SEPs) Observed in the Interplanetary Medium
AU: * Lin, R P
EM: rlin@ssl.berkeley.edu
AF: University of California at Berkeley, Physics Department and Space Sciences Laboratory, Berkeley, CA 94720-7450 United States
AU: Shih, A Y
EM: ayshih@ssl.berkeley.edu
AF: University of California at Berkeley, Physics Department and Space Sciences Laboratory, Berkeley, CA 94720-7450 United States
AU: Krucker, S
EM: krucker@ssl.berkeley.edu
AF: University of California at Berkeley, Space Sciences Laboratory, Berkeley, CA 94720-7450 United States
AU: Smith, D M
EM: dsmith@scipp.ucsc.edu
AF: University of California at Santa Cruz, Physics Department, 1156 High Street, Santa Cruz, CA 95064 United States
AU: Murphy, R
EM: murphy@ssd5.nrl.navy.mil
AF: Naval Research Laboratory, 4555 Overlook Ave Code 7650,, Washington, DC 20375 United States
AU: Share, G
EM: gerald.share@nrl.navy.mil
AF: Naval Research Laboratory, 4555 Overlook Ave Code 7650,, Washington, DC 20375 United States
AU: Mewaldt, R
EM: rmewaldt@srl.caltech.edu
AF: California Institute of Technology, Mail Code 220-47, Pasadena, CA 91125 United States
AU: Cohen, C M
EM: cohen@srl.caltech.edu
AF: California Institute of Technology, Mail Code 220-47, Pasadena, CA 91125 United States
AU: Looper, M D
EM: mark.d.looper@aero.org
AF: The Aerospace Corporation, P.O. Box 92957, Los Angeles, CA 90009 United States
AU: Mason, G M
EM: gmmason@umd.edu
AF: University of Maryland, Department of Physics, College Park, MD 20742 United States
AU: Haggerty, D K
EM: Dennis.Haggerty@jhuapl.edu
AF: Johns Hopkins University-Applied Physics Laboratory, 11100 Johns Hopkins Rd, Laurel, MD 20723-6099 United States
AB: Observations of hard X-ray/gamma-ray continuum and gamma-ray lines produced by energetic electrons and ions, respectively, colliding with the solar atmosphere, have shown that large solar flares can accelerate ions up to many GeV and electrons up to hundreds of MeV. Solar energetic particles (SEPs) are observed by spacecraft near 1 AU and by ground-based instrumentation to extend up to similar energies in large SEP events, but it is believed that a different acceleration process associated with fast Coronal mass Ejections (CMEs) is responsible. The Ramaty High Energy Solar Spectroscopic Imager (RHESSI) mission provides high-resolution spectroscopy and imaging of flare hard X-rays and gamma-rays. Such observations can provide information on the location, energy spectra, and composition of the flare accelerated energetic particles at the Sun. We compare the RHESSI observations of the 2003 October 28, 2003 November 2, and 2005 January 20 flares with both energetic electron and ion observations near 1 AU from ACE, SAMPEX, Wind,and GOES spacecraft, and discuss the implications for the particle acceleration and escape processes
DE: 2118 Energetic particles, solar
DE: 7514 Energetic particles (2114)
DE: 7519 Flares
DE: 7554 X rays, gamma rays, and neutrinos
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2005 Joint Assembly