Seminar

Very—high energy Gamma rays from Galactic SuperNova Remnants

Very—high energy Gamma rays from Galactic SuperNova Remnants Cosmic rays have been studied for more than one century, but their origin is still debated. SuperNova Remnants (SNRs) are often presented as the best candidates for the acceleration of Galactic cosmic rays, up to PeV (=$10^{15}$ eV) energies. Surveys in the very—high gamma—ray range and the numerous detections of SNRs have brought a greater understanding of the physics at SNR shocks, but have not yet provided a irrevocable proof of the SNR hypothesis. This is mainly because two mechanisms, proton-proton interactions and inverse Compton scattering of electrons can often help to explain the observed Gamma rays. By means of Monte—Carlo simulations, it is possible to study Galactic SNRs as a population. When confronting the predictions of our model with actual data from telescopes operating in the TeV range, we can provide a test for the SNR hypothesis. Furthermore, the use of our Monte—Carlo procedure can help to investigate the population accessible by future instruments operating in the multi—TeV range.

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