TeV emission from SN 1006

Supernova 1006 is the first shell type super-nova remnant to show evidence of particle acceleration to TeV energies. In the present paper we examine this possibility by modeling the observed X-ray non-thermal emission in terms of synchrotron radiation from Fermi accelerated electrons. The predicted synchrotron spectrum fits the radio and non-thermal component of the observed soft X-ray to hard X-ray emission quite well. These particles can produce TeV gamma rays by inverse Compton scattering on the microwave radiation and other ambient fields, and the derived electron distribution is also used to calculate the expected inverse Compton flux. We find that if the remnant is characterised by a magnetic field strength lower than ∼ 7µG, then the TeV flux can be higher than that of the Crab Nebula. About 75% of the TeV emission from SN 1006 is expected to be concentrated in the synchrotron bright NE and SW rims (the " hard aegis ") of the remnant, which would allow a sensitive search if the Atmospheric Imaging Cherenkov Technique is used.