4.7 Article

The first days of Type II-P core collapse supernovae in the gamma-ray range

期刊

出版社

OXFORD UNIV PRESS
DOI: 10.1093/mnras/stac217

关键词

supernovae: general; Interstellar medium: cosmic rays; gamma-rays: general

资金

  1. National Science Foundation [1911061]
  2. Villum Fonden [18994]
  3. European Union [847523]
  4. Paris Region Fellowship under the Marie Sklodowska-Curie agreement (project GLADIATOR)
  5. Marie Curie Actions (MSCA) [847523] Funding Source: Marie Curie Actions (MSCA)
  6. Direct For Mathematical & Physical Scien
  7. Division Of Astronomical Sciences [1911061] Funding Source: National Science Foundation

向作者/读者索取更多资源

Type II-P supernovae are the most common core-collapse supernovae that result from the explosions of red supergiant stars. They are potentially effective energetic particle accelerators and can produce gamma-ray signals through the interaction between energetic particles and the surrounding medium. We calculate the gamma-gamma opacity and discuss the time-dependent gamma-ray emissions from Type II-P supernovae. We find that upcoming gamma-ray observatories like the Cherenkov Telescope Array should be able to detect such supernovae in our Galaxy or in the Magellanic Clouds.
Type II-P supernov AE (SNe), the most common core-collapse SNe type, result from the explosions of red supergiant stars. Their detection in the radio domain testifies of the presence of relativistic electrons, and shows that they are potentially efficient energetic particle accelerators. If hadrons can also be accelerated, these energetic particles are expected to interact with the surrounding medium to produce a gamma-ray signal even in the multi-TeV range. The intensity of this signal depends on various factors, but an essential one is the density of the circumstellar medium. Such a signal should however be limited by electron-positron pair production arising from the interaction of the gamma-ray photons with optical photons emitted by the supernova photosphere, which can potentially degrade the gamma-ray signal by over ten orders of magnitude in the first days/weeks following the explosion. We calculate the gamma-gamma opacity from a detailed modelling of the time evolution of the forward shock and supernova photosphere, taking a full account of the non-isotropy of the photon interactions. We discuss the time-dependent gamma-ray TeV emission from Type II-P SNe as a function of the stellar progenitor radius and mass-loss rate, as well as the explosion energy and mass of the ejected material. We evaluate the detectability of the SNe with the next generation of Cherenkov telescopes. We find that, while most extragalactic events may be undetectable, Type II-P SNe exploding in our Galaxy or in the Magellanic Clouds should be detected by gamma-ray observatories such as the upcoming Cherenkov Telescope Array.

作者

我是这篇论文的作者
点击您的名字以认领此论文并将其添加到您的个人资料中。

评论

主要评分

4.7
评分不足

次要评分

新颖性
-
重要性
-
科学严谨性
-
评价这篇论文

推荐

暂无数据
暂无数据