利用引力波估算孤立中子星质量的新方法
A new estimation method for mass of an isolated neutron star using gravitational waves
摘要：
本文研究了利用一颗孤立的快速旋转的中子星（NS）发射的连续引力波（GW）信号估算NS质量的可能性。当GW通过NS的引力势时，GW需要比没有NS时稍微长一点的时间才能到达观察者。这种时间膨胀效应也适用于光子，通常被称为引力时间延迟（或夏皮罗时间延迟）。相应地，由于NS的库仑型引力势，GW的相位从NS偏移，并且所产生的对数相移取决于NS的质量、自旋频率以及到NS的距离。我们表明，NS质量可以，在原则上，通过利用连续GW的两个模式之间的相移差，如一次和两次自旋频率模式引起的自由旋进NS或NS包含一个钉扎的超流核心。我们估计的NS质量的测量精度使用蒙特卡罗模拟和发现的NS的质量与其椭圆率$10^{-6}$在1 kpc通常是可测量的精度$20%$使用爱因斯坦望远镜。
英文摘要：
We investigate a possibility of estimating mass of an isolated rapidly rotating neutron star (NS) from a continuous gravitational wave (GW) signal emitted by the NS. When the GW passes through the gravitational potential of the NS, the GW takes a slightly longer time to travel to an observer than it does in the absence of the NS. Such a time dilation effect holds also for photons and is often referred to as the gravitational time delay (or the Shapiro time delay). Correspondingly, the phase of the GW from the NS shifts due to the Coulomb type gravitational potential of the NS, and the resulting logarithmic phase shift depends on the mass, the spin frequency of the NS, and the distance to the NS. We show that the NS mass can, in principle, be obtained by making use of the phase shift difference between two modes of the continuous GW such as once and twice spin frequency modes induced by a freely precessing NS or a NS containing a pinned superfluid core. We estimate the measurement accuracy of the NS mass using Monte Carlo simulations and find that the mass of the NS with its ellipticity $10^{-6}$ at 1 kpc is typically measurable with an accuracy $20%$ using Einstein Telescope.
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