On the expected gamma-ray emission from nearby flaring stars

Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F68378271%3A_____%2F18%3A00546837" target="_blank" >RIV/68378271:_____/18:00546837 - isvavai.cz</a>
Result on the web
<a href="https://doi.org/10.1093/mnras/stx2806" target="_blank" >https://doi.org/10.1093/mnras/stx2806</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1093/mnras/stx2806" target="_blank" >10.1093/mnras/stx2806</a>

Result language
angličtina
Original language name
On the expected gamma-ray emission from nearby flaring stars
Original language description
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.
Czech name
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Czech description
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Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
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OECD FORD branch
10303 - Particles and field physics

Publication year
2018
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

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