Numerical relativity estimates of the remnant recoil velocity in binary neutron star mergers
Numerical relativity estimates of the remnant recoil velocity in binary neutron star mergers
复制标题
DOI：
10.1103/physrevd.108.103023
复制
发表时间：
2023-08
影响因子：
5
通讯作者：
Sumeet Kulkarni;Surendra Padamata;Anuradha Gupta;D. Radice;R. Kashyap
中科院分区：
文献类型：
--
作者：
Sumeet Kulkarni;Surendra Padamata;Anuradha Gupta;D. Radice;R. Kashyap
我们首次利用数值相对论模拟的数据提出了双中子星合并的反冲速度估计。我们发现，在我们的数据集中，双中子星合并残留物的反冲速度可以达到几十公里/秒的数量级，最高可达150美元/公里/秒。这些后坐力是由于各向异性引力波发射的等效贡献以及合并过程中动态物质的不对称抛射而获得的。我们提供了净反冲速度及其弹射分量作为弹射物质量的函数的拟合，这在通过电磁观测获得弹射物质的约束时可能是有用的。我们还估计了残余物的质量和自旋，发现它们分别在$[2.34,3.38]M_{\odot}$和$[0.63,0.82]$的范围内。
We present, for the first time, recoil velocity estimates for binary neutron star mergers using data from numerical relativity simulations. We find that binary neutron star merger remnants can have recoil velocity of the order of a few tens of km/s and as high as $150$ km/s in our dataset. These recoils are attained due to equivalent contributions from the anisotropic gravitational wave emission as well as the asymmetric ejection of dynamical matter during the merger. We provide fits for net recoil velocity as well as its ejecta component as a function of the amount of ejected matter, which may be useful when constraints on the ejected matter are obtained through electromagnetic observations. We also estimate the mass and spin of the remnants and find them to be in the range $[2.34, 3.38] M_{\odot}$ and $[0.63, 0.82]$ respectively, for our dataset.