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

Foucart, Francois and Haas, Roland and Duez, Matthew D. and O’Connor, Evan and Ott, Christian D. and Roberts, Luke and Kidder, Lawrence E. and Lippuner, Jonas and Pfeiffer, Harald P. and Scheel, Mark A. (2016) Low mass binary neutron star mergers: Gravitational waves and neutrino emission. Physical Review D, 93 (4). Art. No. 044019. ISSN 2470-0010.

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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 powered by r-process nucleosynthesis in neutron-rich material ejected by the merger, and radio emission from the interaction of that ejecta with the interstellar medium. Simulations of these mergers with fully general relativistic codes are critical to understand the merger and postmerger gravitational wave signals and their neutrinos and electromagnetic counterparts. In this paper, we employ the Spectral Einstein Code to simulate the merger of low mass neutron star binaries (two 1.2M⊙ neutron stars) for a set of three nuclear-theory-based, finite temperature equations of state. We show that the frequency peaks of the postmerger gravitational wave signal are in good agreement with predictions obtained from recent 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 time scale 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 (i.e. rapid uniform rotation is sufficient to prevent its collapse). 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.

Item Type:Article
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URLURL TypeDescription Paper
Ott, Christian D.0000-0003-4993-2055
Roberts, Luke0000-0001-7364-7946
Lippuner, Jonas0000-0002-5936-3485
Additional Information:© 2016 American Physical Society. Received 23 October 2015; published 8 February 2016. The authors thank Jan Steinhoff for communicating values for the Love number or the neutron stars used in our simulations, Rodrigo Fernandez and Dan Kasen for useful discussions over the course of this work, and the members of the SxS collaboration for their advice and support. Support for this work was provided by NASA through Einstein Postdoctoral Fellowship Grants No. PF4-150122 (F. F.) and No. PF3-140114 (L. R.) awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under Contract No. NAS8-03060; and through Hubble Fellowship Grant No. 51344.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under Contract No. NAS 5-26555. The authors at CITA gratefully acknowledge support from the NSERC Canada. M. D. D. acknowledges support through NSF Grant No. PHY-1402916. L. K. acknowledges support from NSF Grants No. PHY-1306125 and No. AST-1333129 at Cornell, while the authors at Caltech acknowledge support from NSF Grants No. PHY-1404569, No. AST-1333520, and No. NSF-1440083, and NSF CAREER Award Grant No. PHY-1151197. Authors at both Cornell and Caltech also thank the Sherman Fairchild Foundation for their support. Computations were performed on the supercomputer Briarée from the Université de Montréal, and Guillimin from McGill University, both managed by Calcul Québec and Compute Canada. The operation of these supercomputers is funded by the Canada Foundation for Innovation (CFI), NanoQuébec, RMGA and the Fonds de recherche du Québec—Nature et Technologie (FRQ-NT). Computations were also performed on the Zwicky cluster at Caltech, supported by the Sherman Fairchild Foundation and by NSF Grant No. PHY-0960291. This work also used the Extreme Science and Engineering Discovery Environment (XSEDE) through Grant No. TGPHY990007N, supported by NSF Grant No. ACI-1053575.
Group:TAPIR, Walter Burke Institute for Theoretical Physics
Funding AgencyGrant Number
NASA Einstein Postdoctoral FellowshipPF4-150122
NASA Einstein Postdoctoral FellowshipPF3-140114
NASA Hubble Fellowship51344.001
NASANAS 5-26555
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
Sherman Fairchild FoundationUNSPECIFIED
Canada Foundation for InnovationUNSPECIFIED
Fonds de recherche du Québec-Nature et Technologie (FRQ-NT)UNSPECIFIED
Record Number:CaltechAUTHORS:20160226-081934022
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Official Citation:Low mass binary neutron star mergers: Gravitational waves and neutrino emission Francois Foucart, Roland Haas, Matthew D. Duez, Evan O’Connor, Christian D. Ott, Luke Roberts, Lawrence E. Kidder, Jonas Lippuner, Harald P. Pfeiffer, and Mark A. Scheel Phys. Rev. D 93, 044019 – Published 8 February 2016
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:64789
Deposited By: Tony Diaz
Deposited On:29 Feb 2016 21:48
Last Modified:10 Apr 2017 18:38

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