On the expected gamma-ray emission from nearby flaring stars

0546837 - FZÚ 2022 RIV GB eng J - Článek v odborném periodiku
Ohm, S. … celkem 2 autorů
On the expected gamma-ray emission from nearby flaring stars.
Monthly Notices of the Royal Astronomical Society. Roč. 474, č. 1 (2018), s. 1335-1341. ISSN 0035-8711. E-ISSN 1365-2966
Výzkumná infrastruktura: CTA-CZ - 90046
Klíčová slova: radiation mechanisms: non-thermal * stars: flare * stars: individual: DGCV
Obor OECD: Particles and field physics
Impakt faktor: 5.231, rok: 2018
Způsob publikování: Omezený přístup
https://doi.org/10.1093/mnras/stx2806

Stellar flares have been extensively studied in soft X-rays (SXRs) by basically every X-ray mission. Hard X-ray (HXR) emission from stellar superflares, however, have only been detected from a handful of objects over the past years. One very extreme event was the superflare from the young M-dwarf DGCVn binary star system, which triggered Swift/BAT as if it was a gamma-ray burst. In this work, we estimate the expected gamma-ray emission from DGCVn and the most extreme stellar flares by extrapolating from solar flares based on measured solar energetic particles (SEPs), as well as thermal and non-thermal emission properties. We find that ions are plausibly accelerated in stellar superflares to 100 GeV energies, and possibly up to TeV energies in the associated coronal mass ejections. The corresponding pi(0)-decay gamma-ray emission could be detectable from stellar superflares with ground-based gamma-ray telescopes.
Trvalý link: http://hdl.handle.net/11104/0323223