论文标题
IBN型超新星的特性：对祖细胞进化的影响和快速瞬态的群体的起源
Properties of Type Ibn Supernovae: Implications for the Progenitor Evolution and the Origin of a Population of Rapid Transients
论文作者
论文摘要
IBN型超新星（SNE IBN）显示出Sn射流与氢贫血偶然物质（CSM）之间强烈相互作用的特征。 SNE IBN的射出和CSM性质提供了一个很好的机会来研究大型恒星的最终演变。在目前的工作中，我们提出了一个射流曲线（LC）模型，以考虑到最初在正向上产生的高能光子并将反向冲击转换为光学中观察到的发射的过程。该模型应用于SNE IBN和“ SN IBN”的样本，快速发展。我们表明，在SN IBN LCS中常见的峰值后行为，在缓慢的衰减之后是快速衰减，自然而然地解释了从冷却到绝热状态的过渡而没有引入CSM密度分布的变化。快速衰减阶段（常见的）斜率（常见的）斜率表明陡峭的CSM密度梯度（Rho_csm〜r^{ - 3}），推断出作为SN IBN祖细胞的一般特性的质量损失速率迅速增加。我们认为，从衍生的喷射和CSM性质中，我们认为，最初质量> 18 msun的巨大狼射线星可以是祖细胞的潜在类别。目前的工作还表明，目前缺少的紫外线快速瞬变人群的最终质量损失率低于光学SNE IBN，这可以通过未来的UV任务有效探测。
Type Ibn Supernovae (SNe Ibn) show signatures of strong interaction between the SN ejecta and hydrogen-poor circumstellar matter (CSM). Deriving the ejecta and CSM properties of SNe Ibn provides a great opportunity to study the final evolution of massive stars. In the present work, we present a light curve (LC) model for the ejecta-CSM interaction, taking into account the processes in which the high-energy photons originally created at the forward and reverse shocks are converted to the observed emission in the optical. The model is applied to a sample of SNe Ibn and `SN Ibn' rapidly evolving transients. We show that the characteristic post-peak behavior commonly seen in the SN Ibn LCs, where a slow decay is followed by a rapid decay, is naturally explained by the transition of the forward-shock property from cooling to adiabatic regime without introducing a change in the CSM density distribution. The (commonly-found) slope in the rapid decay phase indicates a steep CSM density gradient (rho_CSM ~ r^{-3}), inferring a rapid increase in the mass-loss rate toward the SN as a generic properties of the SN Ibn progenitors. From the derived ejecta and CSM properties, we argue that massive Wolf-Rayet stars with the initial mass of >~ 18 Msun can be a potential class of the progenitors. The present work also indicates existence of currently missing population of UV-bright rapid transients for which the final mass-loss rate is lower than the optical SNe Ibn, which can be efficiently probed by future UV missions.
