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  Sub-radian-accuracy gravitational waveforms of coalescing binary neutron stars in numerical relativity

Kiuchi, K., Kawaguchi, K., Kyutoku, K., Sekiguchi, Y., Shibata, M., & Taniguchi, K. (2017). Sub-radian-accuracy gravitational waveforms of coalescing binary neutron stars in numerical relativity. Physical Review D, 96: 084060. doi:10.1103/PhysRevD.96.084060.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0004-34DD-9 Version Permalink: http://hdl.handle.net/21.11116/0000-0004-34DE-8
Genre: Journal Article

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 Creators:
Kiuchi, Kenta, Author
Kawaguchi, Kyohei1, Author              
Kyutoku, Koutarou, Author
Sekiguchi, Yuichiro, Author
Shibata, Masaru2, Author              
Taniguchi, Keisuke, Author
Affiliations:
1Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_1933290              
2Computational Relativistic Astrophysics, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_2541714              

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Free keywords: Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE,Astrophysics, Cosmology and Extragalactic Astrophysics, astro-ph.CO,General Relativity and Quantum Cosmology, gr-qc
 Abstract: Extending our previous studies, we perform high-resolution simulations of inspiraling binary neutron stars in numerical relativity. We thoroughly carry through a convergence study in our currently available computational resources with the smallest grid spacing of $\approx 63$--86~meter for the neutron-star radius 10.9--13.7\,km. The estimated total error in the gravitational-wave phase is of order 0.1~rad for the total phase of $\gtrsim 210$\,rad in the last $\sim 15$--16 inspiral orbits. We then compare the waveforms (without resolution extrapolation) with those calculated by the latest effective-one-body formalism (tidal SEOBv2 model referred to as TEOB model). We find that for any of our models of binary neutron stars, the waveforms calculated by the TEOB formalism agree with the numerical-relativity waveforms up to $\approx 3$\,ms before the peak of the gravitational-wave amplitude is reached: For this late inspiral stage, the total phase error is $\lesssim 0.1$\,rad. Although the gravitational waveforms have an inspiral-type feature for the last $\sim 3$\,ms, this stage cannot be well reproduced by the current TEOB formalism, in particular, for neutron stars with large tidal deformability (i.e., lager radius). The reason for this is described.

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 Dates: 2017-08-292017
 Publication Status: Published in print
 Pages: 13 pages, 11 figures, submitted to PRD
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 Rev. Method: -
 Identifiers: arXiv: 1708.08926
DOI: 10.1103/PhysRevD.96.084060
URI: http://arxiv.org/abs/1708.08926
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Title: Physical Review D
  Other : Phys. Rev. D.
Source Genre: Journal
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Publ. Info: Lancaster, Pa. : American Physical Society
Pages: - Volume / Issue: 96 Sequence Number: 084060 Start / End Page: - Identifier: ISSN: 0556-2821
CoNE: https://pure.mpg.de/cone/journals/resource/111088197762258