论文标题
表征带有引力波的天体物理二进制中子星星
Characterizing Astrophysical Binary Neutron Stars with Gravitational Waves
论文作者
论文摘要
合并二进制中子星被认为主要是通过孤立的二进制进化形成的。在这种标准的地层场景中，第一胎中子星经过回收过程，并且在最终的灵感中可能会迅速旋转，而第二颗恒星预计将有效合并时旋转零。基于此功能，我们提出了一个新的框架，用于从其重力波发射中观察到的二进制中子星的天体物理表征。我们进一步提出了回收中子恒星的无量纲旋转的先验，该伽玛分布的形状参数为2，比例参数为0.012，从银河系中性恒星的无线电PULSAR观察结果推断。在标准形成场景的背景下，解释GW170817和GW190425并采用γ-分配之前，我们在非指定假设上找到了积极的支持（贝叶斯因子为6个），对旋转的中子中的旋转中子中的旋转中子中的旋转中心旋转的GW190425中的旋转式旋转率很高。 事先的。我们在GW170817和GW190425中测量回收（慢）中子星的质量为$ 1.34 _ { - 0.09}^{+0.12} $ $（1.38 _ { - 0.11} $ 1.64 _ { - 0.11}^{+0.13} $ $（1.66 _ { - 0.12}^{+0.12}）$ $ M _ {\ odot} $，分别为$ 68 \％$ $。我们讨论了对这两个事件的天体物理起源的影响，并概述了使用我们的框架研究二进制中子星的未来前景。
Merging binary neutron stars are thought to be formed predominantly via isolated binary evolution. In this standard formation scenario, the first-born neutron star goes through a recycling process and might be rapidly spinning during the final inspiral, whereas the second-born star is expected to have effectively zero spin at merger. Based on this feature, we propose a new framework for the astrophysical characterization of binary neutron stars observed from their gravitational wave emission. We further propose a prior for the dimensionless spins of recycled neutron stars, given by a gamma distribution with a shape parameter of 2 and a scale parameter of 0.012, extrapolated from radio pulsar observations of Galactic binary neutron stars. Interpreting GW170817 and GW190425 in the context of the standard formation scenario and adopting the gamma-distribution prior, we find positive support (with a Bayes factor of 6, over the nonspinning hypothesis) for a spinning recycled neutron star in GW190425, whereas the spin of the recycled neutron star in GW170817 is small and consistent with our prior. We measure the masses of the recycled (slow) neutron stars in GW170817 and GW190425 to be $1.34_{-0.09}^{+0.12}$ $(1.38_{-0.11}^{+0.11})$ $M_{\odot}$ and $1.64_{-0.11}^{+0.13}$ $(1.66_{-0.12}^{+0.12})$ $M_{\odot}$, with $68\%$ credibility, respectively. We discuss implications for the astrophysical origins of these two events and outline future prospects of studying binary neutron stars using our framework.
