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#### Viscous evolution of a massive disk surrounding stellar-mass black holes in full general relativity

##### MPS-Authors
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Fujibayashi,  Sho
Computational Relativistic Astrophysics, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

/persons/resource/persons216870

Shibata,  Masaru
Computational Relativistic Astrophysics, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

/persons/resource/persons228206

Wanajo,  Shinya
Computational Relativistic Astrophysics, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

/persons/resource/persons231068

Kiuchi,  Kenta
Computational Relativistic Astrophysics, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

##### External Ressource
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##### Fulltext (public)

2009.03895.pdf
(Preprint), 4MB

PhysRevD.102.123014.pdf
(Publisher version), 8MB

##### Supplementary Material (public)
There is no public supplementary material available
##### Citation

Fujibayashi, S., Shibata, M., Wanajo, S., Kiuchi, K., Kyutoku, K., & Sekiguchi, Y. (2020). Viscous evolution of a massive disk surrounding stellar-mass black holes in full general relativity. Physical Review D, 102(12): 123014. doi:10.1103/PhysRevD.102.123014.

Cite as: http://hdl.handle.net/21.11116/0000-0007-AF75-1
##### Abstract
Long-term viscous neutrino-radiation hydrodynamics simulations in full general relativity are performed for a massive disk surrounding spinning stellar-mass black holes with mass $M_{\rm BH}=4$, $6$, and $10M_\odot$ and initial dimensionless spin $\chi \approx 0.8$. The initial disk is chosen to have mass $M_{\rm disk}\approx 0.1$ or $3M_\odot$ as plausible models of the remnants for the merger of black hole-neutron star binaries or the stellar core collapse from a rapidly rotating progenitor, respectively. For $M_{\rm disk} \approx 0.1M_\odot$ with the outer disk edge initially located at $r_{\rm out} \sim 200$ km, we find that $15$%-$20$% of $M_{\rm disk}$ is ejected and the average electron fraction of the ejecta is $\langle Y_e \rangle = 0.30$-$0.35$ as found in the previous study. For $M_{\rm disk} \approx 3M_\odot$, we find that $\approx 10$%-$20$% of $M_{\rm disk}$ is ejected for $r_{\rm out}\approx 200$-$1000$ km. In addition, $\langle Y_e \rangle$ of the ejecta can be enhanced to be $\gtrsim 0.4$ because the electron fraction is increased significantly during the long-term viscous expansion of the disk with high neutrino luminosity until the mass ejection sets in. Our results suggest that not heavy $r$-process elements but light trans-iron elements would be synthesized in the matter ejected from a massive torus surrounding stellar-mass black holes. We also find that the outcomes of the viscous evolution for the high-mass disk case is composed of a rapidly spinning black hole surrounded by a torus with a narrow funnel, which appears to be suitable for generating gamma-ray bursts.