The first days of Type II-P core collapse supernovae in the gamma-ray range
The first days of Type II-P core collapse supernovae in the gamma-ray range
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伽马射线范围内 II-P 型核心塌陷超新星的第一天
DOI：
10.1093/mnras/stac217
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发表时间：
2022
影响因子：
4.8
通讯作者：
Sol, H.
中科院分区：
文献类型：
--
作者：
Cristofari, P.;Marcowith, A.;Renaud, M.;Dwarkadas, V. V.;Tatischeff, V.;Giacinti, G.;Peretti, E.;Sol, H.
II-P 型超新星 (SNe) 是最常见的核心塌缩 SNe 类型，由红超巨星爆炸产生。它们在无线电领域的检测证明了相对论电子的存在，并表明它们是潜在高效的高能粒子加速器。如果强子也能被加速，这些高能粒子预计将与周围介质相互作用，产生甚至在多 TeV 范围内的伽马射线信号。该信号的强度取决于多种因素，但一个重要因素是星周介质的密度。然而，这种信号应该受到伽马射线光子与超新星光球层发射的光学光子相互作用产生的电子-正电子对的限制，这可能会在爆炸后的最初几天/几周内使伽马射线信号减弱十多个数量级。我们通过对前向激波和超新星光球层的时间演化的详细建模来计算伽马-伽马不透明度，并充分考虑光子相互作用的非各向同性。我们讨论了 II-P 型超新星的随时间变化的伽马射线 TeV 发射，作为恒星前身半径和质量损失率以及爆炸能量和喷射物质质量的函数。我们使用下一代切伦科夫望远镜评估超新星的可探测性。我们发现，虽然大多数河外事件可能无法探测到，但在我们的银河系或麦哲伦云中爆炸的 II-P 型超新星应该可以被伽马射线天文台探测到，例如即将建成的切伦科夫望远镜阵列。
Type II-P supernovæ (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.