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arXiv · 1301.3555

Exploring tidal effects of coalescing binary neutron stars in numerical relativity

Kenta Hotokezaka·Koutarou Kyutoku·Masaru Shibata
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Abstract

We study gravitational waves emitted in the late inspiral stage of binary neutron stars by analyzing the waveform obtained in numerical-relativity simulations. For deriving the physical gravitational waveforms from the numerical results, the resolution extrapolation plays an essential role for our simulations. The extrapolated gravitational-wave phases are compared with those calculated in the post-Newtonian (PN) and effective-one-body (EOB) formalisms including corrections of tidal effects. We show that the extrapolated gravitational-wave phases in numerical relativity agree well with those by the PN and EOB calculations for most of the inspiral stage except for a tidally-dominated, final inspiral stage, in which the PN and EOB results underestimate the tidal effects. Nevertheless, the accumulated phase difference between our extrapolated results and the results by the PN/EOB calculations is at most 1--3 radian in the last 15 cycles.

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Kenta Hotokezaka, Koutarou Kyutoku, Masaru Shibata. 2013-03-07. Exploring tidal effects of coalescing binary neutron stars in numerical relativity. https://doi.org/10.1103/physrevd.87.044001

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