标题： Ibn型超新星的双星起源的人口合成研究 显示英文标题

标题： Population Synthesis Study on the Binary Origin of Type Ibn Supernovae

摘要： 类型 Ibn 超新星（SNe）是一类前身星被密集的富氦周围星际物质（CSM）包围的超新星爆发。 已经提出了几种形成致密 CSM 的模型，有前景的场景包括双星系统中低质量（$\lesssim 3~M_\odot$）氦（He）星，或者 He 星与致密天体之间的共同包层阶段后的合并。 使用快速双星种群合成计算，我们估计了这些通道的事件率，并将其与观测到的 SN Ibn 率进行比较。 我们发现，在近距离双星系统中爆炸的低质量 He 星（分离度为$\lesssim$几个 100 $R_\odot$）可以足够产生以解释观测到的 SN Ibn 事件率，而合并场景可能只能解释其中的一小部分 SNe。 我们讨论了低质量 He 星场景中预期的伴星类型，发现大质量主序星（$10$--$20\ M_\odot$）是典型的，其中可能有相当大的一部分（$<10\%$）双星系统具有白矮星（WD）伴星，其延迟时间长达$100$ Myrs。 显示英文摘要

摘要： Type Ibn supernovae (SNe) are a class of SN explosions whose progenitors are surrounded by dense helium-rich circumstellar matter (CSM). Some models have been proposed for how to form the dense CSM, with promising scenarios involving either binaries with a low-mass ($\lesssim 3~M_\odot$) helium (He) star, or mergers following common envelope phases between a He star and a compact object. Using rapid binary population synthesis calculations, we estimate the event rate of these channels and compare it with the observed SN Ibn rate. We find that exploding low-mass He stars in close binaries (of separations $\lesssim$ a few 100 $R_\odot$) can be sufficiently produced to account for the observed event rate of SN Ibn, while the merger scenario can likely account for only a fraction of these SNe. We discuss the types of companions expected in the low-mass He star scenario, finding massive main sequence stars ($10$--$20\ M_\odot$) to be typical, with a potentially non-negligible fraction ($<10\%$) of binaries with white dwarf (WD) companions that have long delay times of up to $100$ Myrs.