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New viscous neutrino-radiation hydrodynamics simulations are performed foraccretion disks surrounding a spinning black hole with low mass $3M_\odot$ anddimensionless spin 0.8 or 0.6 in full general relativity, aiming at modelingthe evolution of a merger remnant of massive binary neutron stars or low-massblack hole-neutron star binaries. We reconfirm the following results found byprevious studies of other groups: 15-30% of the disk mass is ejected from thesystem with the average velocity of $\sim $5-10% of the speed of light for theplausible profile of the disk as merger remnants. In addition, we find that forthe not extremely high viscous coefficient case, the neutron richness of theejecta does not become very high, because weak interaction processes enhancethe electron fraction during the viscous expansion of the disk before the onsetof the mass ejection, resulting in the suppression of the lanthanide synthesis.For high-mass disks, the viscous expansion timescale is increased by alonger-term neutrino emission, and hence, the electron fraction of the ejectabecomes even higher. We also confirm that the mass distribution of the electronfraction depends strongly on the magnitude of the given viscous coefficient.This demonstrates that a first-principle magnetohydrodynamics simulation isnecessary for black hole-disk systems with sufficient grid resolution and withsufficiently long timescale (longer than seconds) to clarify thenucleosynthesis and electromagnetic signals from them.

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