论文标题
X射线二进制中子星和中子星光洞的诞生
X-raying the Birth of Binary Neutron Stars and Neutron Star-Black Hole Binaries
论文作者
论文摘要
我们考虑在伴随二元中子星（BNS）或中子星形黑色孔二进制（NS-BH）形成的超新星（USSN）之后的后备积聚。后备物质最初会直接吸收到新生的NS，而它开始吸收到电路磁盘，通常为$ 0.1 \ mbox { - } 1 \，\ Mathrm {day} $，在USSN爆炸开始后。环形磁盘质量进一步积聚，在每个紧凑型物体周围形成迷你磁盘，超级 - 埃德丁顿的速率长达几年。我们表明，这样的系统构成了二进制超X射线源（ULX），并且X射线的一部分可以通过USSN弹出物出现。 We encourage follow-up observations of USSNe within $\lesssim 100\,\rm Mpc$ and $\sim 100\mbox{-}1,000\,\mathrm{day}$ after the explosion using Chandra, XMM Newton and NuSTAR, which could detect the X-ray counterpart with time variations representing the properties of the nascent compact binary, e.g., the二进制的轨道运动，NS的自旋和/或迷你磁盘的准碘振荡。
We consider fallback accretion after an ultra-stripped supernova (USSN) that accompanies formation of a binary neutron star (BNS) or a neutron star-black hole binary (NS-BH). The fallback matter initially accretes directly to the nascent NS, while it starts to accrete to the circumbinary disk, typically $0.1\mbox{-}1\, \mathrm{day}$ after the onset of the USSN explosion. The circumbinary disk mass further accretes, forming mini disks around each compact object, with a super-Eddington rate up to a few years. We show that such a system constitutes a binary ultraluminous X-ray source (ULX), and a fraction of the X rays can emerge through the USSN ejecta. We encourage follow-up observations of USSNe within $\lesssim 100\,\rm Mpc$ and $\sim 100\mbox{-}1,000\,\mathrm{day}$ after the explosion using Chandra, XMM Newton and NuSTAR, which could detect the X-ray counterpart with time variations representing the properties of the nascent compact binary, e.g., the orbital motion of the binary, the spin of the NS, and/or the quasiperiodic oscillation of the mini disks.
