期刊
PHYSICAL REVIEW LETTERS
卷 105, 期 26, 页码 -出版社
AMER PHYSICAL SOC
DOI: 10.1103/PhysRevLett.105.261101
关键词
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资金
- DFG [SFB/Transregio 7]
- CompStar
- JSPS [19-07803]
- MEXT [22740163]
- NASA [NNX09AI75G]
- Grants-in-Aid for Scientific Research [22740163] Funding Source: KAKEN
- NASA [117537, NNX09AI75G] Funding Source: Federal RePORTER
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.
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