论文标题
最终紧凑型残余物在20到40 $ m_ \ odot $：下质量差距中
Final compact remnants in core-collapse supernovae from 20 to 40 $M_\odot$: the lower mass gap
论文作者
论文摘要
X射线二进制观测值建议，即“较低的质量差距”提出了$ \ sim 2-5〜m_ \ odot $范围内的紧凑对象的大规模稀少。引力波检测已解锁了另一种质量测量方法，而Aligo/处女座观察到了间隙中的一些候选者。我们以$ \ sim 20-40〜m_ \ odot $祖先星星的身份重新审视核心折叠超新星（CCSNE）上的数值模拟，其初始爆炸能量不同。结果，较低的爆炸能量自然会导致低金属祖先的效率更有效的后备积聚，然后在CCSNE中心的新生黑孔（BHS）可以从间隙中逸出，但是中子星无法轻松地倒入差距中的BHS中。然而，太阳金属祖先的最后残留物始终存在于差距上。如果我们认为只能观察到剧烈的CCSNE，并且那些爆炸能量较低的人是通用的，那么较低的质量间隙就可以合理地建造。间隙的宽度和深度主要取决于典型的CCSN初始爆炸能量和金属性。可以预期，未来的多信子观察紧凑对象描述了间隙的形状，这可能会限制CCSNE及其祖细胞的特性。
A mass paucity of compact objects in the range of $\sim 2-5 ~M_\odot$ has been suggested by X-ray binary observations, namely, the "lower mass gap". Gravitational wave detections have unlocked another mass measurement method, and aLIGO/Virgo has observed some candidates in the gap. We revisit the numerical simulations on the core-collapse supernovae (CCSNe) for $\sim 20-40~M_\odot$ progenitor stars with differently initial explosion energies. As a result, the lower explosion energy naturally causes more efficient fallback accretion for low-metallicity progenitors, and then the newborn black holes (BHs) in the center of the CCSNe can escape from the gap, but neutron stars cannot easily collapse into BHs in the gap; nevertheless, the final remnants of the solar-metallicity progenitors stick to the gap. If we consider that only drastic CCSNe can be observed and that those with lower explosion energies are universal, the lower mass gap can be reasonably built. The width and depth of the gap are mainly determined by the typical CCSN initial explosion energy and metallicity. One can expect that the future multi-messenger observations of compact objects delineate the shape of the gap, which might constrain the properties of the CCSNe and their progenitors.
