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

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 $M_{\mathrm{BH}}=4$, $6$, and $10M_{\odot }$ and initial dimensionless spin $\chi \approx 0.8$. The initial disk is chosen to have mass $M_{\mathrm{disk}}\approx 0.1$ 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 $M_{\mathrm{disk}}\approx 0.1M_{\odot }$ with the outer disk edge initially located at $r_{\mathrm{out}}\sim 200$ km, we find that $15$%-$20$% of $M_{\mathrm{disk}}$ is ejected and the average electron fraction of the ejecta is $⟨Y_e⟩=0.30$-$0.35$ as found in the previous study. For $M_{\mathrm{disk}}\approx 3M_{\odot }$, we find that $\approx 10$%-$20$% of $M_{\mathrm{disk}}$ is ejected for $r_{\mathrm{out}}\approx 200$-$1000$ km. In addition, $⟨Y_e⟩$ 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.

25 pages, 17 figures

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