论文标题
GW190814：中子星伴侣的旋转和方程
GW190814: Spin and equation of state of a neutron star companion
论文作者
论文摘要
Ligo/处女座最近发现的合并二进制文件具有$ \ sim 23 m_ \ odot $黑洞和$ \ sim 2.6 m_ \ odot $ compact companion引发了有关次要的性质的辩论，该性质属于所谓的质量差距。在这里，我们探讨了次级是中子星（NS）的假设的一些后果。我们以迄今为止可行的状态方程（EOSS）的具体例子表明，某些EOSS不需要快速均匀的旋转，而其他人则不足以解释NS的存在。从GW170817衍生的球形NS的最大质量的绝对上限已经表明，这种未知的紧凑型伴侣可能是缓慢甚至不旋转的NS。但是，GW170817偏爱的几个软ns Eoss，最大球形质量$ \ lyseSim 2.1 m_ \ odot $不能被调用以解释该对象，即使允许最大均匀旋转。相比之下，足够僵硬的eoss产生了$ 2.6 m_ \ odot $ nss，又缓慢旋转，或者在某些情况下是不旋转的，并且与GW170817兼容，并且更好的结果可以解释Black Hole Companion。
The recent discovery by LIGO/Virgo of a merging binary having a $\sim 23 M_\odot$ black hole and a $\sim 2.6 M_\odot$ compact companion has triggered a debate regarding the nature of the secondary, which falls into the so-called mass gap. Here we explore some consequences of the assumption that the secondary was a neutron star (NS). We show with concrete examples of heretofore viable equations of state (EOSs) that rapid uniform rotation may neither be necessary for some EOSs nor sufficient for others to explain the presence of a NS. Absolute upper limits for the maximum mass of a spherical NS derived from GW170817 already suggest that this unknown compact companion might be a slowly or even a nonrotating NS. However several soft NS EOSs favored by GW170817 with maximum spherical masses $\lesssim 2.1 M_\odot$ cannot be invoked to explain this object, even allowing for maximum uniform rotation. By contrast, sufficiently stiff EOSs that yield $2.6 M_\odot$ NSs which are slowly rotating or, in some cases, nonrotating, and are compatible with GW170817 and the results of NICER, can account for the black hole companion.
