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  Low mass binary neutron star mergers : gravitational waves and neutrino emission

Foucart, F., Haas, R., Duez, M. D., O'Connor, E., Ott, C. D., Roberts, L., et al. (2016). Low mass binary neutron star mergers: gravitational waves and neutrino emission. Physical Review D, 93: 044019. doi:10.1103/PhysRevD.93.044019.

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Item Permalink: http://hdl.handle.net/11858/00-001M-0000-002A-6DE6-7 Version Permalink: http://hdl.handle.net/21.11116/0000-0002-EBBB-3
Genre: Journal Article

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 Creators:
Foucart, Francois, Author
Haas, Roland1, Author              
Duez, Matthew D., Author
O'Connor, Evan, Author
Ott, Christian D., Author
Roberts, Luke, Author
Kidder, Lawrence E., Author
Lippuner, Jonas, Author
Pfeiffer, Harald P., Author
Scheel, Mark A., Author
Affiliations:
1Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_1933290              

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Free keywords: Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE,General Relativity and Quantum Cosmology, gr-qc
 Abstract: Neutron star mergers are among the most promising sources of gravitational waves for advanced ground-based detectors. These mergers are also expected to power bright electromagnetic signals, in the form of short gamma-ray bursts, infrared/optical transients, and radio emission. Simulations of these mergers with fully general relativistic codes are critical to understand the merger and post-merger gravitational wave signals and their neutrinos and electromagnetic counterparts. In this paper, we employ the SpEC code to simulate the merger of low-mass neutron star binaries (two $1.2M_\odot$ neutron stars) for a set of three nuclear-theory based, finite temperature equations of state. We show that the frequency peaks of the post-merger gravitational wave signal are in good agreement with predictions obtained from simulations using a simpler treatment of gravity. We find, however, that only the fundamental mode of the remnant is excited for long periods of time: emission at the secondary peaks is damped on a millisecond timescale in the simulated binaries. For such low-mass systems, the remnant is a massive neutron star which, depending on the equation of state, is either permanently stable or long-lived. We observe strong excitations of l=2, m=2 modes, both in the massive neutron star and in the form of hot, shocked tidal arms in the surrounding accretion torus. We estimate the neutrino emission of the remnant using a neutrino leakage scheme and, in one case, compare these results with a gray two-moment neutrino transport scheme. We confirm the complex geometry of the neutrino emission, also observed in previous simulations with neutrino leakage, and show explicitly the presence of important differences in the neutrino luminosity, disk composition, and outflow properties between the neutrino leakage and transport schemes.

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 Dates: 2015-10-212016-01-222016
 Publication Status: Published in print
 Pages: Accepted by PRD; 23 pages; 24 figures; 4 tables
 Publishing info: -
 Table of Contents: -
 Rev. Method: -
 Identifiers: arXiv: 1510.06398
DOI: 10.1103/PhysRevD.93.044019
URI: http://arxiv.org/abs/1510.06398
 Degree: -

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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: 93 Sequence Number: 044019 Start / End Page: - Identifier: ISSN: 0556-2821
CoNE: /journals/resource/111088197762258