Relationship of Solar Flare Accelerated Particles to Solar Energetic Particles (SEPs) Observed in the Interplanetary Medium

Details Relationship of Solar Flare Accelerated Particles to Solar Energetic Particles (SEPs) Observed in the Interplanetary Medium Relationship of Solar Flare Accelerated Particles to Solar Energetic Particles (SEPs) Observed in the Interplanetary Medium

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsh33a..02l&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SH33A-02

Physics

2118 Energetic Particles, Solar, 7514 Energetic Particles (2114), 7519 Flares, 7554 X Rays, Gamma Rays, And Neutrinos

Scientific paper

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

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