Radiation hydrodynamical simulations of eruptive mass loss from progenitors of Type Ibn/IIn supernovae
Radiation hydrodynamical simulations of eruptive mass loss from progenitors of Type Ibn/IIn supernovae
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DOI：
10.1051/0004-6361/201937226
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发表时间：
2019-12
影响因子：
6.5
通讯作者：
Naoto Kuriyama;T. Shigeyama
中科院分区：
文献类型：
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作者：
Naoto Kuriyama;T. Shigeyama
上下文。观测表明，一些大质量恒星经历了与显著变亮相关的剧烈和爆发的质量损失，这是无法用流体静力恒星模型解释的。这个事件似乎形成了致密的星际物质(CSM)。喷发质量损失的机制还没有完全解释清楚。我们关注的事实是，对于一些大质量恒星来说，在核心崩塌前几年，核燃烧的时间尺度比包络的动力学时间尺度要短。目标。为了揭示喷发质量损失的性质，我们研究了它与核内部发生的核燃烧所提供的包层底部的能量注入的关系。在这项研究中，我们没有具体说明将能量从核燃烧地点传输到信封底部的实际机制。取而代之的是，我们将注入能量的量和注入时间参数化，并试图从与观察值的比较中提取关于这些参数的信息。方法：研究方法。我们对红、黄、蓝超巨星以及Wolf-Rayet恒星的前身进行了一维辐射流体力学模拟。我们用一个公开的恒星演化代码计算了祖先的演化。结果。我们得到了与喷发有关的光曲线、抛射质量的量以及核坍塌时的CSM分布。结论。大质量恒星包层底部的能量注入时间短于包层的动力学时间尺度，可以重现核心崩塌前的一些观测到的光学爆发，并形成CSM，它可以为被归类为IIn类型的相互作用超新星提供动力。
Context. Observations suggest that some massive stars experience violent and eruptive mass loss associated with significant brightening that cannot be explained by hydrostatic stellar models. This event seemingly forms dense circumstellar matter (CSM). The mechanism of eruptive mass loss has not been fully explained. We focus on the fact that the timescale of nuclear burning gets shorter than the dynamical timescale of the envelope a few years before core collapse for some massive stars. Aims. To reveal the properties of the eruptive mass loss, we investigate its relation to the energy injection at the bottom of the envelope supplied by nuclear burning taking place inside the core. In this study, we do not specify the actual mechanism for transporting energy from the site of nuclear burning to the bottom of the envelope. Instead, we parameterize the amount of injected energy and the injection time and try to extract information on these parameters from comparisons with observations. Methods. We carried out 1D radiation hydrodynamical simulations for progenitors of red, yellow, and blue supergiants, and Wolf–Rayet stars. We calculated the evolution of the progenitors with a public stellar evolution code. Results. We obtain the light curve associated with the eruption, the amount of ejected mass, and the CSM distribution at the time of core-collapse. Conclusions. The energy injection at the bottom of the envelope of a massive star within a period shorter than the dynamical timescale of the envelope could reproduce some observed optical outbursts prior to the core-collapse and form the CSM, which can power an interaction supernova classified as Type IIn.