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

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.

19 pages, 2 figures, 1 table. Comments are welcome

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Cited by in corpus (6)

• Orbital decay of double white dwarfs: beyond gravitational wave radiation effects
• A gamma-ray study of galactic PeVatron candidates LHAASO J1825-1326 and LHAASO J1839-0545
• Prospects for gamma-ray emission from magnetar regions in CTAO observations
• An updated view and perspectives on high-energy gamma-ray emission from SGR J1935+2154 and its environment
• Massive Star Clusters as sources of high-energy gamma radiation
• The Fast Radio Burst-emitting magnetar SGR 1935+2154 -- proper motion and variability from long-term Hubble Space Telescope monitoring