论文标题
重越好：如何限制高质量中子星级合并的质量比和旋转
The heavier the better: how to constrain mass ratios and spins of high-mass neutron-star mergers
论文作者
论文摘要
第一个二进制中子合并事件GW170817及其明亮的电磁对应物提供了大量的信息。相比之下，第二个事件是$ m _ {\ rm tot} = 3.4^{+0.3} _ { - 0.1} \，m _ {\ odot} $，并且缺乏电磁对应物，我们对中子形式的理解很难改善我们对中子形式的理解。尽管GW190425与合并导致迅速崩溃的场景兼容，并迅速崩溃，几乎没有弹出的物质为对应物提供动力，从而确定了质量比和二元的有效旋转$ \ tilde的，仍然很难。这是因为重力波形还不能很好地限制二进制的组件旋转。但是，由于GW190425的质量明显大于非旋转中子星的最大质量，因此$ m _ {_ {_ {\ rm tov}} $ $ Q $ $ q $不能太小，因为较重的恒星不会重力稳定。利用普遍关系和大量状态方程式，我们提供了GW190425的$（\tildeχ，Q）$飞机，即：$ q _ {\ rm min} \ geq 0.38 $和$ \ \ \ \ \ \ \ \ \ \tildeχ_ 3.4 \，m_ \ odot $。最后，我们展示了高质量二进制文件的未来观察如何在$ m _ {_ {\ rm tov}} $上提供下限。
The first binary neutron-star merger event, GW170817, and its bright electromagnetic counterpart have provided a remarkable amount of information. By contrast, the second event, GW190425, with $M_{\rm tot}=3.4^{+0.3}_{-0.1}\,M_{\odot}$ and the lack of an electromagnetic counterpart, has hardly improved our understanding of neutron-star physics. While GW190425 is compatible with a scenario in which the merger has lead to a prompt collapse to a black hole and little ejected matter to power a counterpart, determining the mass ratio and the effective spin $\tildeχ$ of the binary remains difficult. This is because gravitational waveforms cannot yet well constrain the component spins of the binary. However, since the mass of GW190425 is significantly larger than the maximum mass for nonrotating neutron stars, $M_{_{\rm TOV}}$, the mass ratio $q$ cannot be too small, as the heavier star would not be gravitationally stable. Making use of universal relations and a large number of equations of state, we provide limits in the $(\tildeχ,q)$ plane for GW190425, namely: $q_{\rm min} \geq 0.38$ and $ \tildeχ_{\rm max}\leq 0.20$, assuming $M_\mathrm{tot} \simeq 3.4\, M_\odot$. Finally, we show how future observations of high-mass binaries can provide a lower bound on $M_{_{\rm TOV}}$.
