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  Neutrino transport in black hole-neutron star binaries: neutrino emission and dynamical mass ejection

Kyutoku, K., Kiuchi, K., Sekiguchi, Y., Shibata, M., & Taniguchi, K. (2018). Neutrino transport in black hole-neutron star binaries: neutrino emission and dynamical mass ejection. Physical Review D, 97: 023009. doi:10.1103/PhysRevD.97.023009.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0000-B040-0 Version Permalink: http://hdl.handle.net/21.11116/0000-0000-B0E4-7
Genre: Journal Article

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 Creators:
Kyutoku, Koutarou, Author
Kiuchi, Kenta, Author
Sekiguchi, Yuichiro, 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
 Abstract: We study the merger of black hole-neutron star binaries by fully general-relativistic neutrino-radiation-hydrodynamics simulations throughout the coalescence, particularly focusing on the role of neutrino irradiation in dynamical mass ejection. Neutrino transport is incorporated by an approximate transfer scheme based on the truncated moment formalism. While we fix the mass ratio of the black hole to the neutron star to be 4 and the dimensionless spin parameter of the black hole to be 0.75, the equations of state for finite-temperature neutron-star matter are varied. The hot accretion disk formed after tidal disruption of the neutron star emits a copious amount of neutrinos with the peak total luminosity ~1--3x10^53 erg s^(-1) via thermal pair production and subsequent electron/positron captures on free nucleons. Nevertheless, the neutrino irradiation does not modify significantly the electron fraction of the dynamical ejecta from the neutrinoless beta-equilibrium value at zero temperature of initial neutron stars. The mass of the wind component driven by neutrinos from the remnant disk is negligible compared to the very neutron-rich dynamical component, throughout our simulations performed until a few tens milliseconds after the onset of merger, for the models considered in this study. These facts suggest that the ejecta from black hole-neutron star binaries are very neutron rich and are expected to accommodate strong r-process nucleosynthesis, unless magnetic or viscous processes contribute substantially to the mass ejection from the disk. We also find that the peak neutrino luminosity does not necessarily increase as the disk mass increases, because tidal disruption of a compact neutron star can result in a remnant disk with a small mass but high temperature.

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 Dates: 2017-10-022018-01-212018
 Publication Status: Published in print
 Pages: 17 pages, 16 figures, matched to the published version
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 Table of Contents: -
 Rev. Method: -
 Identifiers: arXiv: 1710.00827
DOI: 10.1103/PhysRevD.97.023009
URI: http://arxiv.org/abs/1710.00827
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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: 97 Sequence Number: 023009 Start / End Page: - Identifier: ISSN: 0556-2821
CoNE: /journals/resource/111088197762258