Dependence of the gamma-ray emission from SN 1006 on the astronomical parameters

Abstract

We use nonlinear kinetic theory to study the remnant dynamics and the particle acceleration as well as the properties of the nonthermal emission from the supernova remnant SN 1006. The known range of astronomical parameters is examined to determine whether it encompasses the existing synchrotron emission data. Given the present-day spatial extent and expansion rate of the object, it is shown that the hadronic gamma-ray flux is very sensitive to the ambient gas density N_H and that the existing H.E.S.S. upper limit requires N_H < 0.1 cm^{-3}. The strength of the amplified magnetic field downstream of the shock is about 150 μG.

10 pages, 8 figures, to be published in Astronomy and Astrophysics

References in corpus (2)

• Confirmation of strong magnetic field amplification and nuclear cosmic ray acceleration in SN 1006
• Variation of cosmic ray injection across supernova shocks

Cited by in corpus (9)

• First detection of VHE gamma-rays from SN 1006 by H.E.S.S
• Theory of cosmic ray production in the supernova remnant RX J1713.7-3946
• The gas density around SN 1006
• The First X-Ray Proper-Motion Measurements of the Forward Shock in the Northeastern Limb of SN 1006
• Evidence of a Curved Synchrotron Spectrum in the Supernova Remnant SN 1006
• Cosmic Ray Acceleration by Supernova Shocks
• Hadronic versus leptonic origin of the gamma-ray emission from Supernova Remnant RX J1713.7-3946
• Observational Evidence for Magnetic Field Amplification in SN 1006
• New Results from High Energy Gamma-Ray Astronomy