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 MBH=4, 6, and 10 M⊙ and initial dimensionless spin χ≈0.8. The initial disk is chosen to have mass Mdisk≈0.1 or 3 M⊙ 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 Mdisk≈0.1 M⊙ with the outer disk edge initially located at rout∼200 km, we find that 15%-20% of Mdisk is ejected and the average electron fraction of the ejecta is ⟨Ye