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  Revisiting the lower bound on tidal deformability derived by AT 2017gfo

Kiuchi, K., Kyutoku, K., Shibata, M., & Taniguchi, K. (submitted). Revisiting the lower bound on tidal deformability derived by AT 2017gfo.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0003-576B-4 Version Permalink: http://hdl.handle.net/21.11116/0000-0003-5770-D
Genre: Journal Article

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 Creators:
Kiuchi, Kenta, Author
Kyutoku, Koutarou, Author
Shibata, Masaru1, Author              
Taniguchi, Keisuke, Author
Affiliations:
1Computational 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,General Relativity and Quantum Cosmology, gr-qc,Nuclear Theory, nucl-th
 Abstract: We revisit the lower bound on binary tidal deformability tilde{Lambda} imposed by a luminous kilonova/macronova, AT 2017gfo, by numerical-relativity simulations of models consistent with gravitational waves from the binary-neutron-star merger, GW170817. Contrary to the claim made in the literature, we find that binaries with tilde{Lambda}<~400 can explain the luminosity of AT 2017gfo as far as moderate mass ejection from the remnant is assumed as also done in the previous work. The reason is that the maximum mass of a neutron star is not strongly correlated with tidal deformability of neutron stars with typical mass of ~1.4M_sun. If the maximum mass is so large that the binary does not collapse to a black hole immediately after merger, the mass of the ejecta can be sufficiently large irrespective of the binary tidal deformability. We explicitly present models of binary mergers with tilde{Lambda} down to 242 that satisfy the requirement on the mass of the ejecta from the luminosity of AT 2017gfo. We further find that the luminosity of AT 2017gfo could even be explained by models that do not experience bounce after merger. We conclude that the luminosity of AT 2017gfo is not very useful to constrain the binary tidal deformability. Accurate estimation of the mass ratio will be necessary to put a lower bound using electromagnetic counterparts in the future. We also caution that merger simulations performed employing a limited class of tabulated equations of state could be severely biased due to the lack of generality.

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 Dates: 2019-03-042019-03-112019
 Publication Status: Submitted
 Pages: 6 pages, 2 figures
 Publishing info: -
 Table of Contents: -
 Rev. Method: -
 Identifiers: arXiv: 1903.01466
URI: http://arxiv.org/abs/1903.01466
 Degree: -

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Title: Astrophysical Journal
Source Genre: Journal
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Publ. Info: Chicago, IL : University of Chicago Press for the American Astronomical Society
Pages: - Volume / Issue: - Sequence Number: - Start / End Page: - Identifier: ISSN: 0004-637X
CoNE: https://pure.mpg.de/cone/journals/resource/954922828215_2