The next generation of ground-based interferometric gravitational wave detectors will observe mergers of black holes and neutron stars throughout cosmic time. A large number of the binary neutron star merger events will be observed with extreme high fidelity, and will provide stringent constraints on the equation of state of nuclear matter. In this paper, we investigate the systematic improvement in the measurability of the equation of state with increase in detector sensitivity by combining constraints obtained on the radius of a 1.4M⊙ neutron star from a simulated source population. Since the measurability of the equation of state depends on its stiffness, we consider a range of realistic equations of state that span the current observational constraints. We show that a single 40 km Cosmic Explorer detector can pin down the neutron star radius for a soft, medium and stiff equation of state with a precision of 10 m within a decade, whereas the current generation of ground-based detectors like the Advanced LIGO-Virgo network would take O(105) years to do so for a soft equation of state.

中文翻译：

---

使用第二代和第三代引力波探测器网络测量中子星半径


下一代地基干涉引力波探测器将在整个宇宙时间内观测黑洞和中子星的合并。大量的双中子星合并事件将以极高的保真度进行观测，并将对核物质的状态方程提供严格的约束。在本文中，我们通过结合从模拟源群中获得的对 1.4M⊙ 中子星半径的约束，研究了状态方程可测量性随着探测器灵敏度的增加而得到的系统性改进。由于状态方程的可测量性取决于其刚度，因此我们考虑了一系列跨越当前观测约束的现实状态方程。我们表明，单个 40 公里的宇宙探测器可以在十年内以 10 m 的精度确定软、中和硬状态方程的中子星半径，而当前一代的地面探测器，如先进的 LIGO-Virgo 网络，需要 O（105） 年才能完成软状态方程。