High-energy gamma-ray emission from SNR G57.2+0.8 hosting SGR J1935+2154
| Autor: | Jonas P. Pereira, Jaziel G. Coelho, R. C. Anjos, Fernando Catalani |
|---|---|
| Rok vydání: | 2021 |
| Předmět: |
Physics
High Energy Physics - Theory High Energy Astrophysical Phenomena (astro-ph.HE) High energy Astrophysics::High Energy Astrophysical Phenomena Galactic Center Soft gamma repeater Gamma ray FOS: Physical sciences Astronomy and Astrophysics Astrophysics Particle acceleration Supernova Acceleration High Energy Physics - Phenomenology High Energy Physics - Phenomenology (hep-ph) Astrophysics - Solar and Stellar Astrophysics High Energy Physics - Theory (hep-th) Astrophysics - High Energy Astrophysical Phenomena Energy (signal processing) Astrophysics::Galaxy Astrophysics Solar and Stellar Astrophysics (astro-ph.SR) |
| DOI: | 10.48550/arxiv.2106.03008 |
| Popis: | 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 |
| Databáze: | OpenAIRE |
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