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Analytic modelling of tidal effects in the relativistic inspiral of binary neutron stars

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Rezzolla,  Luciano
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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1009.0521
(Preprint), 540KB

PRL105_261101.pdf
(Any fulltext), 909KB

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Citation

Baiotti, L., Damour, T., Giacomazzo, B., Nagar, A., & Rezzolla, L. (2010). Analytic modelling of tidal effects in the relativistic inspiral of binary neutron stars. Physical Review Letters, 105: 261101. doi:10.1103/PhysRevLett.105.261101.

Cite as: http://hdl.handle.net/11858/00-001M-0000-000E-EF84-C
Abstract
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 $\simeq 22$ GW cycles are $\Delta \phi\simeq \pm 0.24$ 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.