The Origin of High Energy Cosmic-Ray Electrons and nearby Supernova Remnants

Details The Origin of High Energy Cosmic-Ray Electrons and nearby Supernova Remnants The Origin of High Energy Cosmic-Ray Electrons and nearby Supernova Remnants

Jul 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003icrc....4.1993y&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

We calculated the energy spectrum of cosmic-ray electrons in a semianalityc approach by separating the contributions of distant and nearby sources, using the observed local SNRs in the neighb orhood of the solar system. In this calculation, we considered the case that the accelerated electrons are lib erated from the SNR after ˜ 103 - 105 yr from the explosion. The electron spectrum from the source is assumed to be a power-law with an exponential cut-off. From this calculation, we found that some observed nearby SNRs leave unique signatures in the form of identifiable structure in the energy spectrum of TeV electrons. This suggests that, in addition to providing information on the mechanisms of acceleration and propagation of cosmic-rays, specific cosmic-ray sources can be identified through the precise observation of electrons in the TeV region.

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