NONTHERMAL EMISSION OF SUPERNOVA REMNANT SN 1006 REVISITED: THEORETICAL MODEL AND THE H.E.S.S. RESULTS

The properties of the Galactic supernova remnant (SNR) SN 1006 are theoretically re-analyzed in light of the recent H.E.S.S. results. The physical parameters of the model-proton injection rate, electron-to-proton ratio, and downstream magnetic field strength-are determined through a fit of the result to the observed spatially integrated synchrotron emission properties. The only remaining unknown astronomical parameter, the circumstellar gas number density, is determined by a normalization of the amplitude of the [gamma]-ray flux to the observed amplitude. The hadronic and leptonic [gamma]-ray emissions are of comparable strength. The overall energy of accelerated CRs at the present epoch is of the order of 5% of the total hydrodynamic explosion energy, and is predicted to rise with time by a factor of approximately 2. The sum of the results suggests that SN 1006 is a CR source with a high efficiency of nuclear CR production, as required for the Galactic CR sources, both in flux as well as in cutoff energy.