Mass ejection from the merger of binary neutron stars
Mass ejection from the merger of binary neutron stars
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DOI：
10.1103/physrevd.87.024001
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发表时间：
2012-12
影响因子：
5
通讯作者：
K. Hotokezaka;K. Kiuchi;K. Kyutoku;Hirotada Okawa;Y. Sekiguchi;M. Shibata;K. Taniguchi
中科院分区：
文献类型：
--
作者：
K. Hotokezaka;K. Kiuchi;K. Kyutoku;Hirotada Okawa;Y. Sekiguchi;M. Shibata;K. Taniguchi
数值相对论模拟的合并双中子星进行各种状态方程（EOS）和合理的范围内的中子星质量，主要集中在从系统中喷出的物质的属性。我们发现一小部分物质以相对论性和各向异性的方式被喷射出来，其典型速度和最大速度分别为0.15 - 0.25c和0.5 - 0.8c（其中$c$是光速），总的喷射静止质量在一个很宽的范围$10^{-4}$ -$10^{-2}M_{\odot}$，这强烈地依赖于EOS，总质量和质量比。喷射出的总动能也在10 ^{49}$和10 ^{51} {\rm ergs}$之间的宽范围内。数值计算结果表明，对于总质量为2.7M $的双星，如果物态方程和双星的质量是有利的，则外流可以通过r$-过程产生重元素不稳定核或通过与星际物质相互作用形成冲击波而产生电磁信号，从而被计划中的望远镜观测到.
Numerical-relativity simulations for the merger of binary neutron stars are performed for a variety of equations of state (EOSs) and for a plausible range of the neutron-star mass, focusing primarily on the properties of the material ejected from the system. We find that a fraction of the material is ejected as a mildly relativistic and mildly anisotropic outflow with the typical and maximum velocities $\sim 0.15$ -- $0.25c$ and $\sim 0.5$ -- $0.8c$ (where $c$ is the speed of light), respectively, and that the total ejected rest mass is in a wide range $10^{-4}$ -- $10^{-2}M_{\odot}$, which depends strongly on the EOS, the total mass, and the mass ratio. The total kinetic energy ejected is also in a wide range between $10^{49}$ and $10^{51} {\rm ergs}$. The numerical results suggest that for a binary of canonical total mass $2.7M_{\odot}$, the outflow could generate an electromagnetic signal observable by the planned telescopes through the production of heavy-element unstable nuclei via the $r$-process or through the formation of blast waves during the interaction with the interstellar matter, if the EOS and mass of the binary are favorable ones.