Analytic Modeling of Tidal Effects in the Relativistic Inspiral of Binary Neutron Stars

被引：119

作者：

Baiotti, Luca ^{[1
,2
]}

Damour, Thibault ^{[3
,4
]}

Giacomazzo, Bruno ^{[5
,6
,7
]}

Nagar, Alessandro ^{[3
]}

Rezzolla, Luciano ^{[7
,8
]}

机构：

[1] Osaka Univ, Inst Laser Engn, Suita, Osaka, Japan

[2] Kyoto Univ, Yukawa Inst Theoret Phys, Kyoto 606, Japan

[3] Inst Hautes Etud Sci, F-91440 Bures Sur Yvette, France

[4] ICRANet, Pescara, Italy

[5] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[6] NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA

[7] Albert Einstein Inst, Max Planck Inst Gravitat Phys, Potsdam, Germany

[8] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA

来源：

PHYSICAL REVIEW LETTERS | 2010年 / 105卷 / 26期

关键词：

D O I：

10.1103/PhysRevLett.105.261101

中图分类号：

O4 [物理学];

学科分类号：

0702 ;

摘要：

To detect the gravitational-wave (GW) signal from binary neutron stars and extract information about the equation of state of matter at nuclear density, it is necessary to match the signal with a bank of accurate templates. We present the two longest (to date) general-relativistic simulations of equal-mass binary neutron stars with different compactnesses, C = 0.12 and C = 0.14, and compare them with a tidal extension of the effective-one-body (EOB) model. The typical numerical phasing errors over the similar or equal to 22 GW cycles are Delta phi similar or equal to +/- 0.24 rad. By calibrating only one parameter (representing a higher-order amplification of tidal effects), the EOB model can reproduce, within the numerical error, the two numerical waveforms essentially up to the merger. By contrast, the third post-Newtonian Taylor-T4 approximant with leading-order tidal corrections dephases with respect to the numerical waveforms by several radians.

引用

页数：4

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