Physics
Scientific paper
Jul 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003icrc....6.3335v&link_type=abstract
Proceedings of the 28th International Cosmic Ray Conference. July 31-August 7, 2003. Trukuba, Japan. Under the auspices of the I
Physics
Scientific paper
Recent observational evidence from soft X-ray imaging data supports models of coronal shock wave propagation in the solar atmosphere as freely propagating blast waves, which refract toward the solar surface as they propagate away from the flare site. We have modeled particle acceleration in such a refracting large-scale solar coronal shock wave. The geometry of such a shock wave results in the observer in the interplanetary medium being magnetically connected with the downstream region of the shock wave. Thus, the accelerated particles escape to the observer through the region of shocked plasma behind the shock front, which may explain why the energy spectrum observed in the interplanetary medium is usually a power-law. Using parameters of upstream turbulence obtained from models of a cyclotron-heated solar corona we show that the particle acceleration model results in proton energy spectra generally consistent with those frequently observed in small, gradual solar energetic particle events. In addition, this process can serve as a pre-acceleration mechanism for further acceleration in CME-driven shocks in large gradual events.
Khan Josef I.
Vainio Rami O.
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