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Black hole-neutron star mergers using a survey of finite-temperature equations of state

Brege, Wyatt and Duez, Matthew D. and Foucart, Francois and Deaton, M. Brett and Caro, Jesus and Hemberger, Daniel A. and Kidder, Lawrence E. and O’Connor, Evan and Pfeiffer, Harald P. and Scheel, Mark A. (2018) Black hole-neutron star mergers using a survey of finite-temperature equations of state. Physical Review D, 98 (6). Art. No. 063009. ISSN 2470-0010. doi:10.1103/physrevd.98.063009.

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Each of the potential signals from a black hole–neutron star merger should contain an imprint of the neutron star equation of state: gravitational waves via its effect on tidal disruption, the kilonova via its effect on the ejecta, and the gamma-ray burst via its effect on the remnant disk. These effects have been studied by numerical simulations and quantified by semianalytic formulas. However, most of the simulations on which these formulas are based use equations of state without finite temperature and composition-dependent nuclear physics. In this paper, we simulate black hole–neutron star mergers varying both the neutron star mass and the equation of state, using three finite-temperature nuclear models of varying stiffness. Our simulations largely vindicate formulas for ejecta properties but do not find the expected dependence of disk mass on neutron star compaction. We track the early evolution of the accretion disk, largely driven by shocking and fallback inflow, and do find notable equation-of-state effects on the structure of this early-time, neutrino-bright disk.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Duez, Matthew D.0000-0002-0050-1783
Foucart, Francois0000-0003-4617-4738
Kidder, Lawrence E.0000-0001-5392-7342
Pfeiffer, Harald P.0000-0001-9288-519X
Additional Information:© 2018 American Physical Society. Received 26 April 2018; published 12 September 2018. The authors thank Roland Haas and the members of the SXS Collaboration for helpful discussions over the course of this project. M. D. acknowledges support through NSF Grants No. PHY-1402916 and PHY-1806207. Support for this work was provided by NASA through Einstein Postdoctoral Fellowship Grant No. PF4-150122 (F. F.) awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under Contract No. NAS8-03060. H. P. gratefully acknowledges support from the NSERC Canada, the Canada Research Chairs Program and the Canadian Institute for Advanced Research. L. K. acknowledges support from NSF Grants No. PHY-1708212 and PHY-1708213 at Cornell, while the authors at Caltech acknowledge support from NSF Grants No. PHY-1404569, and NSF-1440083. 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, 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 and Wheeler clusters at Caltech, supported by the Sherman Fairchild Foundation and by NSF Award No. PHY-0960291.
Group:TAPIR, Walter Burke Institute for Theoretical Physics
Funding AgencyGrant Number
NASA Einstein FellowshipPF4-150122
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
Canada Research Chairs ProgramUNSPECIFIED
Canadian Institute for Advanced Research (CIFAR)UNSPECIFIED
Sherman Fairchild FoundationUNSPECIFIED
Canada Foundation for InnovationUNSPECIFIED
Fonds de recherche du Québe-Nature et technologies (FRQ-NT)UNSPECIFIED
Issue or Number:6
Record Number:CaltechAUTHORS:20180912-081414077
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:89552
Deposited By: Tony Diaz
Deposited On:12 Sep 2018 16:57
Last Modified:16 Nov 2021 00:36

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