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 $1.4 \, \mathrm{M}_{\odot}$ 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 40km Cosmic Explorer detector can pin down the neutron star radius for a soft, medium and stiff equation of state to an accuracy of 10m within a decade, whereas the current generation of ground-based detectors like the Advanced LIGO-Virgo network would take $\mathcal{O}(10^5)$ years to do so for a soft equation of state.
Measuring the delay time distribution of binary neutron stars. II. Using the redshift distribution from third-generation gravitational wave detectors network
Measuring radii of merging neutron stars with interface-mode asteroseismology informed by nuclear theory and experiment
University of Bath（巴斯大学）；East Texas A&M University（东德克萨斯农工大学）；Texas A&M University（德克萨斯农工大学）；Ohio University（俄亥俄大学）；Michigan State University（密歇根州立大学）；CNRS（法国国家科学研究中心）
Measuring accretion disc properties in the transitional millisecond pulsar PSR J1023+0038 using XMM-Newton, NuSTAR, NICER and Chandra
Indian Institute of Technology Hyderabad（印度理工学院海得拉巴分校）；Tata Institute of Fundamental Research（塔塔基础研究所）；Massachusetts Institute of Technology（麻省理工学院）；Indian Institute of Science Education and Research, Pune（印度科学教育与研究学院浦那分校）
