Measuring neutron-star radii with gravitational-wave detectors -: art. no. 231102

被引：65

作者：

Faber, JA ^{[1
]}

Grandclément, P

Rasio, FA

Taniguchi, K

机构：

[1] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA

[2] Univ Tokyo, Dept Earth Sci & Astron, Tokyo 1538902, Japan

来源：

PHYSICAL REVIEW LETTERS | 2002年 / 89卷 / 23期

基金：

美国国家科学基金会;

关键词：

D O I：

10.1103/PhysRevLett.89.231102

中图分类号：

O4 [物理学];

学科分类号：

0702 ;

摘要：

Coalescing binary neutron stars (NS) are expected to be an important source of gravitational waves (GW) detectable by laser interferometers. We present here a simple method for determining the compactness ratio M/R of NS based on the observed deviation of the GW energy spectrum from point-mass behavior at the end of inspiral. Our method is based on the properties of quasiequilibrium binary NS sequences and does not require the computation of the full GW signal h(t). Combined with the measurement of the NS masses during inspiral, the determination of M/R will allow very strong constraints to be placed on the equation of state of dense nuclear matter.

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