Dark Age of Type II Supernova Remnants
Dark Age of Type II Supernova Remnants
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DOI：
10.3847/2041-8213/ac24ac
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发表时间：
2021-09
期刊：
影响因子：
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通讯作者：
H. Yasuda;Shiu-Hang Lee;K. Maeda
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文献类型：
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作者：
H. Yasuda;Shiu-Hang Lee;K. Maeda
超新星遗迹与超新星爆发机制、祖星和宇宙线加速等都有着密切的联系，是重要的天体。SNRs的非热辐射是探测其周围星周介质（CSM）结构的有效手段，它可以揭示大质量恒星难以捉摸的质量损失的机制和历史。在这项工作中，我们计算的时间演变的宽带非热发射SNRs起源于II型SNe嵌入在CSM环境中链接的质量损失历史的祖先。我们的研究结果预测，II型信噪比经历了一个长期的弱无线电和γ射线发射，如果他们遇到一个空间扩展的泡沫低密度和高温的恒星风在主序星。对于一个在平均星际介质中演化的典型红超巨星祖先来说，这个“黑暗年龄”对应的信噪比年龄范围从1000年到5000年。这一结果表明，大多数II型SNRs太微弱而无法被检测到，这可能有助于解释为什么已知的银河系SNRs的数量明显少于我们对银河系SN率的预期。
Supernova remnants (SNRs) are important objects in terms of their connections with supernova (SN) explosion mechanism(s), progenitor stars, and cosmic-ray acceleration. Nonthermal emission from SNRs is an effective probe of the structure of their surrounding circumstellar media (CSM), which can in turn shed lights on the mechanism and history of the elusive mass loss of massive stars. In this work, we calculate the time evolution of broadband nonthermal emission from SNRs originating from Type II SNe embedded in a CSM environment linked to the mass-loss history of the progenitor. Our results predict that Type II SNRs experience a prolonged period of weak radio and γ-ray emission if they run into a spatially extended bubble of low density and high temperature created by the stellar wind during main sequence. For a typical red supergiant progenitor evolved within an average interstellar medium, this “dark age” corresponds to a range of SNR ages spanning from ∼1000 to 5000 yr old. This result suggests that a majority of Type II SNRs are too faint to be detected, which may help explain why the number of known Galactic SNRs is significantly less than what we expect from the SN rate in our Galaxy.