论文标题
低质量IB/C超新星祖细胞的极端质量损失
Extreme mass loss in low-mass type Ib/c supernova progenitors
论文作者
论文摘要
观察到许多核心塌陷超新星（SNE）具有良好的氢和低质量喷射（例如超脱落的SNE和IBN SNE型）与密集的室内材料（CSM）相互作用。这些事件可能是由于氦星的核心爆发而引起的，这些氦气被二元同伴大量剥离，并在其生命的最后几周弹出了巨大的质量。在氦星模型到核心崩溃之前的几天中，我们确定了一系列氦气核质量$ \ \ \ 2.5 -3 m _ {\ odot} $，其信封的膨胀是由于氦壳燃烧而大大扩展的，而核心经历了霓虹灯和氧气燃烧。在二进制系统中建模时，这些氦星的快速扩展会引起晚期大传输的极高速率（$ \ dot {m} \ gtrsim 10^{ - 2} m_ \ odot/{\ odot/{\ rm yr yr} $）在核心爆发前的几周开始。我们考虑了在这些系统中生产CSM的两种情况：质量转移保持稳定，质量损失是从积聚伴侣附近的系统驱动的，或者传质变为不稳定，并导致氦封膜不绑定的共同信封事件（CEE）。随后的CSM属性与CSM质量（$ \ sim 10^{ - 2} -1 m_ \ odot $）和radii（$ \ sim 10^{13} -10} -10^{16} {\ rm cm cm} $）推断了Ultra-Stripped SNE和几个类型IBN SNE。此外，经历CEE的系统可能会产生短周期的NS二进制文件，在不到100 Myr的情况下合并。
Many core collapse supernovae (SNe) with hydrogen-poor and low-mass ejecta, such as ultra-stripped SNe and type Ibn SNe, are observed to interact with dense circumstellar material (CSM). These events likely arise from the core-collapse of helium stars which have been heavily stripped by a binary companion and ejected significant mass during the last weeks to years of their lives. In helium star models run to days before core-collapse, we identify a range of helium core masses $\approx 2.5 -3 M_{\odot}$ whose envelopes expand substantially due to helium shell burning while the core undergoes neon and oxygen burning. When modeled in binary systems, the rapid expansion of these helium stars induces extremely high rates of late-stage mass transfer ($\dot{M} \gtrsim 10^{-2} M_\odot/{\rm yr}$) beginning weeks to decades before core-collapse. We consider two scenarios for producing CSM in these systems: either mass transfer remains stable and mass loss is driven from the system in the vicinity of the accreting companion, or mass transfer becomes unstable and causes a common envelope event (CEE) through which the helium envelope is unbound. The ensuing CSM properties are consistent with the CSM masses ($\sim 10^{-2}-1 M_\odot$) and radii ($\sim 10^{13}-10^{16} {\rm cm}$) inferred for ultra-stripped SNe and several type Ibn SNe. Furthermore, systems that undergo a CEE could produce short-period NS binaries that merge in less than 100 Myr.
