Exploring the sensitivity of gravitational wave detectors to neutron star physics
Exploring the sensitivity of gravitational wave detectors to neutron star physics
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DOI：
10.1103/physrevd.99.102004
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发表时间：
2019-01
影响因子：
5
通讯作者：
D. Martynov;H. Miao;Han Yang;F. Vivanco;E. Thrane;Rory Smith;P. Lasky;W. East;R. Adhikari;A. Bauswein;A. Brooks;Yanbei Chen;T. Corbitt;H. Grote;Y. Levin;Chunnong Zhao;A. Vecchio
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文献类型：
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作者：
D. Martynov;H. Miao;Han Yang;F. Vivanco;E. Thrane;Rory Smith;P. Lasky;W. East;R. Adhikari;A. Bauswein;A. Brooks;Yanbei Chen;T. Corbitt;H. Grote;Y. Levin;Chunnong Zhao;A. Vecchio
中子星的物理学可以用聚结的双星系统发出的引力波来研究。潮汐效应在最后几个轨道上变得很明显，在500赫兹以上的引力波频谱中可以看到。合并后，中子星残骸以高于1千赫的频率振荡，并可能坍塌成黑洞。引力波探测器在2-4千赫频率下的灵敏度为$\ensuremath{\simeq}{10}^{\ensuremath{-}24}\text{}\TEXT{}\MATHROM{SRACTURE}/\SQRT{\MATHROM{HZ}}$，可以在大约100MPC以外的源上观测到这些振荡。目前的观测站，如LIGO和VIRGO，都受到高频散粒噪声的限制，在3 kHz时的灵敏度大于或等于$2\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}23}\text{。在本文中，我们提出了一种引力波探测器的光学结构，它可以利用现有的干涉仪拓扑结构在现有的设备上安装。该方案有可能在不影响探测器对黑洞二进制的灵敏度的情况下，在2.5 kHz的频率下达到$7\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}25}\text{。我们认为，拟议的仪器有可能探测到与下一代探测器(如宇宙探测器和爱因斯坦望远镜)类似的合并后中子星振荡。我们还对未来的中子星物理探测器的臂长进行了优化，发现最优的臂长为$\ensureath{\约x}20\Text{}\mathm{Km}$。这些仪器有可能以每年约30次事件的速度观测中子星合并后的振荡，信噪比为5或更高。
The physics of neutron stars can be studied with gravitational waves emitted from coalescing binary systems. Tidal effects become significant during the last few orbits and can be visible in the gravitational wave spectrum above 500 Hz. After the merger, the neutron star remnant oscillates at frequencies above 1 kHz and can collapse into a black hole. Gravitational wave detectors with a sensitivity of $\ensuremath{\simeq}{10}^{\ensuremath{-}24}\text{ }\text{ }\mathrm{strain}/\sqrt{\mathrm{Hz}}$ at 2--4 kHz can observe these oscillations from a source which is approximately 100 Mpc away. The current observatories, such as LIGO and Virgo, are limited by shot noise at high frequencies and have a sensitivity of greater than or equal to $2\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}23}\text{ }\text{ }\mathrm{strain}/\sqrt{\mathrm{Hz}}$ at 3 kHz. In this paper, we propose an optical configuration of gravitational wave detectors, which can be set up in present facilities using the current interferometer topology. This scheme has the potential to reach $7\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}25}\text{ }\text{ }\mathrm{strain}/\sqrt{\mathrm{Hz}}$ at 2.5 kHz without compromising the detector sensitivity to black hole binaries. We argue that the proposed instruments have the potential to detect similar amount of postmerger neutron star oscillations as the next generation detectors, such as Cosmic Explorer and Einstein Telescope. We also optimize the arm length of the future detectors for neutron star physics and find that the optimal arm length is $\ensuremath{\approx}20\text{ }\text{ }\mathrm{km}$. These instruments have the potential to observe neutron star postmerger oscillations at a rate of approximately 30 events per year with a signal-to-noise ratio of 5 or more.