TeV Gamma-Rays from Old Supernova Remnants

Details TeV Gamma-Rays from Old Supernova Remnants TeV Gamma-Rays from Old Supernova Remnants

Mar 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007ebhe.conf..205y&link_type=abstract

ENERGY BUDGET IN THE HIGH ENERGY UNIVERSE . Proceedings of the International Workshop. Held 22-24 February 2006 in Kashiwa, Japa

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Scientific paper

We study the emission from an old supernova remnant (SNR) with an age of around 105 yrs. When the SNR age is around 105 yrs, hadron acceleration is efficient enough to emit TeV γ-rays at the shock of the SNR. The maximum energy of primarily accelerated electrons is so small that TeV γ-rays and X-rays are dominated by hadronic processes, π0-decay and synchrotron radiation from secondary electrons, respectively. However, if the SNR is older than several 105 yrs, there are few high-energy particles emitting TeV γ-rays because of the energy loss effect and/or the wave damping effect occurring at low-velocity isothermal shocks. It is found that the ratio of TeV γ-ray (1-10 TeV) to X-ray (2-10 keV) energy flux can be more than ˜ 102. Such a source showing large flux ratio may be a possible origin of recently discovered unidentified TeV sources.

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