• acceleration of particles;
  • radiation mechanisms: non-thermal;
  • stars: individual: SN 1006;
  • cosmic rays;
  • ISM: supernova remnants


Images of SN 1006 have a number of important properties. For instance, the bright limbs coincide spatially in various bands, they have different brightnesses, and the contrast of brightness varies from radio to gamma rays. The reasons for such properties and the role of the magnetic field strength are discussed. Simple, almost model-independent methods and analytical approximations for the derivation of the strength of the magnetic field from the comparison of radio, X-ray and TeV images of the supernova remnant are presented. The methods require the TeV image to be well resolved and accurate, at least to the level of the radio and X-ray maps, so that reasonable constraints can be placed on the magnetic field. If we apply the methods to the present HESS data, they limit the strength of the magnetic field in the limbs of SN 1006 to values lower than a few hundred micro-gauss. If applied to the Fermi-LAT band, the model predicts the same position and same ratio of the surface brightness for GeV photons as for the radio band. We conclude that future TeV and GeV high-resolution data may prove to be very informative about the magnetic field of SN 1006.