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  Mass ejection from disks surrounding a low-mass black hole: Viscous neutrino-radiation hydrodynamics simulation in full general relativity

Fujibayashi, S., Shibata, M., Wanajo, S., Kiuchi, K., Kyutoku, K., & Sekiguchi, Y. (2020). Mass ejection from disks surrounding a low-mass black hole: Viscous neutrino-radiation hydrodynamics simulation in full general relativity. Physical Review D, 101: 083029. doi:10.1103/PhysRevD.101.083029.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0006-630A-0 Version Permalink: http://hdl.handle.net/21.11116/0000-0006-630E-C
Genre: Journal Article

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 Creators:
Fujibayashi, Sho1, Author              
Shibata, Masaru1, Author              
Wanajo, Shinya1, Author              
Kiuchi, Kenta1, Author              
Kyutoku, Koutarou, Author
Sekiguchi, Yuichiro, 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
 Abstract: New viscous neutrino-radiation hydrodynamics simulations are performed for accretion disks surrounding a spinning black hole with low mass $3M_\odot$ and dimensionless spin 0.8 or 0.6 in full general relativity, aiming at modeling the evolution of a merger remnant of massive binary neutron stars or low-mass black hole-neutron star binaries. We reconfirm the following results found by previous studies of other groups: 15-30% of the disk mass is ejected from the system with the average velocity of $\sim $5-10% of the speed of light for the plausible profile of the disk as merger remnants. In addition, we find that for the not extremely high viscous coefficient case, the neutron richness of the ejecta does not become very high, because weak interaction processes enhance the electron fraction during the viscous expansion of the disk before the onset of the mass ejection, resulting in the suppression of the lanthanide synthesis. For high-mass disks, the viscous expansion timescale is increased by a longer-term neutrino emission, and hence, the electron fraction of the ejecta becomes even higher. We also confirm that the mass distribution of the electron fraction depends strongly on the magnitude of the given viscous coefficient. This demonstrates that a first-principle magnetohydrodynamics simulation is necessary for black hole-disk systems with sufficient grid resolution and with sufficiently long timescale (longer than seconds) to clarify the nucleosynthesis and electromagnetic signals from them.

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 Dates: 2020-01-132020
 Publication Status: Published in print
 Pages: 26 pages, 15 figures, to be submitted to PRD
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 Rev. Method: -
 Identifiers: arXiv: 2001.04467
DOI: 10.1103/PhysRevD.101.083029
URI: http://arxiv.org/abs/2001.04467
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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: 101 Sequence Number: 083029 Start / End Page: - Identifier: ISSN: 0556-2821
CoNE: https://pure.mpg.de/cone/journals/resource/111088197762258