Emission of SN 1006 produced by accelerated cosmic rays

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  • 4 April 2002
Abstract
The nonlinear kinetic model of cosmic ray (CR) acceleration in supernova remnants (SNRs) is used to describe the properties of the remnant of SN 1006. It is shown, that the theory fits the existing data in a satisfactory way within a set of parameters which is consistent with the idea that SN 1006 is a typical Galactic CR source. The adjusted parameters are those that are not very well determined by present theory or not directly amenable to astronomical observations. The calculated expansion law and the radio-, X-ray and gamma-ray emissions produced by the accelerated CRs in SN 1006 agree quite well with the observations. A quite large interior magnetic field of about 0.1 mG is required to give a good fit for the radio and X-ray synchrotron emission. In the observed TeV gamma-ray flux from SN 1006, the pion-decay gamma-rays, generated by the nuclear CR component, dominate over the inverse Compton (IC) gamma-rays, generated by the CR electrons in the cosmic microwave background. The predicted hard integral gamma-ray flux extends up to energies ~ 100 TeV if CR diffusion is as strong as the Bohm limit. Only if the interior magnetic field is much lower, ~ 0.01 mG, then the observed gamma-ray emission is due to the accelerated electron component alone. In this case, less plausible physically in our view, the upper limit of the proton to electron ratio is so low (less than 5), and their maximum individual energy and total energy content so small, that SN 1006 can not be considered as a typical source of the Galactic CRs.

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