论文标题
发光的快速蓝色光学瞬变和类型的IBN/ICN SNE，来自狼射线/黑洞合并
Luminous Fast Blue Optical Transients and Type Ibn/Icn SNe from Wolf-Rayet/Black Hole Mergers
论文作者
论文摘要
挑战快速蓝色光学瞬变（LFBOTS;原型：AT2018COW）的“发光”子类的祖细胞模型，以同时解释其所有观察到的特性：快速光学上升时间<days <days <days <days <days <days <days <days <days <days <days <days <days <days。峰值发光度> 1E44 ERG/S;低产量<0.1 msun 56ni；具有较大速度范围的非球形喷射（<3000 km/s至> 0.1-0.5 c，极性纬度增加）；在径向尺度上存在氢耗尽但无用的浓室内材料（CSM），从〜1E14 cm到〜3E16 cm；非热X射线/伽马射线的嵌入式变量来源，暗示着一个紧凑的对象。我们表明，所有这些特性都与黑洞（BH）或中子星（NS）二进制伴侣对沃尔夫射线（WR）星的潮汐破坏和超胆汁一致。与相关的先前模型相反，合并是在公共信封（CE）事件之后长时间延迟（> 〜100年），这是导致二进制造成二进制的事件，这是由于逐渐的角动量损失到遗物环形磁盘上。从合并生成的积聚流中流出的磁盘流出产生了具有必要速度范围的56ni poor非球形喷射。尽管CSM冲击相互作用也有贡献，但光曲线主要是通过重新处理X射线来驱动的。主要CSM来源包括合并最早（〜<1E14 cm）和Relic CE CE磁盘及其光蒸发驱动的风（> 〜1E16 cm）的最早合并阶段（〜<1E14 cm）中的WR星（例如，L2点）的质量损失。更长的延迟合并可能会引起超新星类型的IBN/ICN（取决于WR进化状态），可能会将这些瞬态类别与LFBOTS连接起来。
Progenitor models for the "luminous" subclass of Fast Blue Optical Transients (LFBOTs; prototype: AT2018cow) are challenged to simultaneously explain all of their observed properties: fast optical rise times < days; peak luminosities >1e44 erg/s; low yields <0.1 Msun of 56Ni; aspherical ejecta with a wide velocity range (<3000 km/s to > 0.1-0.5 c with increasing polar latitude); presence of hydrogen-depleted-but-not-free dense circumstellar material (CSM) on radial scales from ~1e14 cm to ~3e16 cm; embedded variable source of non-thermal X-ray/gamma-rays, suggestive of a compact object. We show that all of these properties are consistent with the tidal disruption and hyper-accretion of a Wolf-Rayet (WR) star by a black hole (BH) or neutron star (NS) binary companion. In contrast with related previous models, the merger occurs with a long delay (>~ 100 years) following the common envelope (CE) event responsible for birthing the binary, as a result of gradual angular momentum loss to a relic circumbinary disk. Disk-wind outflows from the merger-generated accretion flow generate the 56Ni-poor aspherical ejecta with the requisite velocity range. The optical light curve is powered primarily by reprocessing X-rays from the inner accretion flow/jet, though CSM shock interaction also contributes. Primary CSM sources include mass-loss from WR star (e.g., from the L2 point) during the earliest stages of the merger (~<1e14 cm) and the relic CE disk and its photoevaporation-driven wind (>~ 1e16 cm). Longer delayed mergers may instead give rise to supernovae Type Ibn/Icn (depending on the WR evolutionary state), potentially connecting these transient classes with LFBOTs.
