Neutron-Star Radius from a Population of Binary Neutron Star Mergers

被引：92

作者：

Bose, Sukanta ^{[1
,2
]}

Chakravarti, Kabir ^{[1
]}

Rezzolla, Luciano ^{[3
,4
]}

Sathyaprakash, B. S. ^{[5
,6
,7
]}

Takami, Kentaro ^{[3
,8
]}

机构：

[1] Interuniv Ctr Astron & Astrophys, Post Bag 4, Pune 411007, Maharashtra, India

[2] Washington State Univ, Dept Phys & Astron, 1245 Webster, Pullman, WA 99164 USA

[3] Inst Theoret Phys, Max von Laue Str 1, D-60438 Frankfurt, Germany

[4] Frankfurt Inst Adv Studies, Ruth Moufang Str 1, D-60438 Frankfurt, Germany

[5] Penn State Univ, Phys Dept, Inst Gravitat & Cosmos, University Pk, PA 16802 USA

[6] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA

[7] Cardiff Univ, Sch Phys & Astron, 5 Parade, Cardiff CF24 3AA, S Glam, Wales

[8] Kobe City Coll Technol, Kobe, Hyogo 6512194, Japan

来源：

PHYSICAL REVIEW LETTERS | 2018年 / 120卷 / 03期

基金：

欧洲研究理事会; 美国国家科学基金会;

关键词：

Relativity - Gravitational effects - Stars - Errors - Neutrons - Gravity waves;

D O I：

10.1103/PhysRevLett.120.031102

中图分类号：

O4 [物理学];

学科分类号：

0702 ;

摘要：

We show how gravitational-wave observations with advanced detectors of tens to several tens of neutron-star binaries can measure the neutron-star radius with an accuracy of several to a few percent, for mass and spatial distributions that are realistic, and with none of the sources located within 100 Mpc. We achieve such an accuracy by combining measurements of the total mass from the inspiral phase with those of the compactness from the postmerger oscillation frequencies. For estimating the measurement errors of these frequencies, we utilize analytical fits to postmerger numerical relativity waveforms in the time domain, obtained here for the first time, for four nuclear-physics equations of state and a couple of values for the mass. We further exploit quasiuniversal relations to derive errors in compactness from those frequencies. Measuring the average radius to well within 10% is possible for a sample of 100 binaries distributed uniformly in volume between 100 and 300 Mpc, so long as the equation of state is not too soft or the binaries are not too heavy. We also give error estimates for the Einstein Telescope.

引用

页数：6

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