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High-energy gamma-ray emission from SNR G57.2+0.8 hosting SGR J1935+2154 (2106.03008v3)

Published 6 Jun 2021 in astro-ph.HE, astro-ph.SR, hep-ph, and hep-th

Abstract: In recent years some efforts have been made to identify active sources capable of accelerating particles up to $10{15}$ eV, known as PeVatrons. Measurements of TeV ($10{12}$ eV) gamma-rays from supernova remnants (SNRs) have shown that efficient particle acceleration can occur in SNR diffusive shocks. In this paper, we obtain the contribution to the high energy and very-high-energy gamma-ray (VHE, $E > 100$ GeV) emission due to cosmic-ray acceleration from SNR G57.2+0.8 hosting the Soft Gamma Repeater (SGR) J1935+2154 with the use of the GALPROP code. To do so, we take into account the SNR + SGR association as a single source close to the Galactic center. We propose that the above setting can provide a more comprehensive scenario for the generation of GeV-TeV gamma-rays. We also discuss the contribution from the SNR G57.2+0.8 and SGR J1935+2154 region to the diffusive TeV energy gamma-ray emission from the Galactic center.

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