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Model comparison from LIGO-Virgo data on GW170817's binary components and consequences for the merger remnant

The LIGO Scientific Collaboration, The Virgo Collaboration, Abbott, B. P., Abbott, R., Abbott, T. D., Abraham, S., et al. (in preparation). Model comparison from LIGO-Virgo data on GW170817's binary components and consequences for the merger remnant.

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1908.01012.pdf (Preprint), 876KB
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1908.01012.pdf
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### Creators

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Creators:
The LIGO Scientific Collaboration, Author
The Virgo Collaboration, Author
Abbott, B. P., Author
Abbott, R., Author
Abbott, T. D., Author
Abraham, S., Author
Acernese, F., Author
Ackley, K., Author
Affeldt, C.1, Author
Agathos, M., Author
Agatsuma, K., Author
Aggarwal, N., Author
Aguiar, O. D., Author
Aiello, L., Author
Ain, A., Author
Ajith, P., Author
Allen, G., Author
Allocca, A., Author
Affiliations:
1Laser Interferometry & Gravitational Wave Astronomy, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, ou_24010
2Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_1933290
3Observational Relativity and Cosmology, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, ou_24011
4Binary Merger Observations and Numerical Relativity, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, ou_2461691
5Computational Relativistic Astrophysics, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_2541714
6AEI-Golm, MPI for Gravitational Physics, Max Planck Society, Golm, DE, ou_24008

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Free keywords: General Relativity and Quantum Cosmology, gr-qc, Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE
Abstract: GW170817 is the very first observation of gravitational waves originating from the coalescence of two compact objects in the mass range of neutron stars, accompanied by electromagnetic counterparts, and offers an opportunity to directly probe the internal structure of neutron stars. We perform Bayesian model selection on a wide range of theoretical predictions for the neutron star equation of state. For the binary neutron star hypothesis, we find that we cannot rule out the majority of theoretical models considered. In addition, the gravitational-wave data alone does not rule out the possibility that one or both objects were low-mass black holes. We discuss the possible outcomes in the case of a binary neutron star merger, finding that all scenarios from prompt collapse to long-lived or even stable remnants are possible. For long-lived remnants, we place an upper limit of 1.9 kHz on the rotation rate. If a black hole was formed any time after merger and the coalescing stars were slowly rotating, then the maximum baryonic mass of non-rotating neutron stars is at most 3.05 \$M_\odot\$, and three equations of state considered here can be ruled out. We obtain a tighter limit of 2.67 \$M_\odot\$ for the case that the merger results in a hypermassive neutron star.

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Dates: 2019-08-022019-08-14
Publication Status: Not specified
Pages: 35 pages, 4 figures
Publishing info: -
Rev. Method: -
Identifiers: arXiv: 1908.01012
URI: http://arxiv.org/abs/1908.01012
Degree: -

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