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K.K. Dyer, S.P. Reynolds (NCSU)
Galactic cosmic rays up to energies of around 1015 eV are assumed to originate in supernova remnants (SNRs). The shock wave of a young SNR like SN 1006 can accelerate electrons to energies of greater than 1 TeV, where they can produce synchrotron radiation into the X-ray band. Our previous studies showed that several detailed models could describe adequately the X-ray data available at the time. The models invoke different values for the magnetic-field strength and electron scattering properties, with different implications for the acceleration of the unseen ions which are expected to dominate the cosmic-ray energetics. New observations by ASCA, ROSAT, and RXTE have enormously improved both the amount and quality of the data, and have also extended to higher X-ray energies. These data should allow much firmer constraints on models, and may rule out current versions. We will describe model fits to these new data, emphasizing the physical constraints that can be placed on SNRs and on the cosmic-ray acceleration process.
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