• DOI:10.1103/PhysRevD.84.024017
• Corpus ID: 56216396

Accurate numerical simulations of inspiralling binary neutron stars and their comparison with effective-one-body analytical models

@article{Baiotti2011AccurateNS,
  title={Accurate numerical simulations of inspiralling binary neutron stars and their comparison with effective-one-body analytical models},
  author={Luca Baiotti and T. Damour and Bruno Giacomazzo and Alessandro Nagar and Luciano Rezzolla},
  journal={Physical Review D},
  year={2011},
  volume={84},
  pages={024017}
}

• L. Baiotti, T. Damour, +2 authors L. Rezzolla
• Published 20 March 2011
• Physics
• Physical Review D

Binary neutron-star systems represent one of the most promising sources of gravitational waves. In order to be able to extract important information, notably about the equation of state of matter at nuclear density, it is necessary to have in hand an accurate analytical model of the expected waveforms. Following our recent work [L. Baiotti, T. Damour, B. Giacomazzo, A. Nagar, and L. Rezzolla, Phys. Rev. Lett. 105, 261101 (2010).], we here analyze more in detail two general-relativistic simulations spanning about 20 gravitational-wave cycles of the inspiral of equal-mass binary neutron stars with different compactnesses, and compare them with a tidal extension of the effective-one-body (EOB) analytical model. The latter tidally extended EOB model is analytically complete up to the 1.5 post-Newtonian level, and contains an analytically undetermined parameter representing a higher-order amplification of tidal effects. We find that, by calibrating this single parameter, the EOB model can reproduce, within the numerical error, the two numerical waveforms essentially up to the merger. By contrast, analytical models (either EOB or Taylor-T4) that do not incorporate such a higher-order amplification of tidal effects, build a dephasing with respect to the numerical waveforms of several radians.