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We present the first numerical result of fully general relativisticaxisymmetric simulations for the collapse of a rotating high-entropy stellarcore to a black hole and an accretion disk. The simulations are performedtaking into account the relevant microphysics. We adopt as initial condition aspherical core with constant electron fraction ($Y_e = 0.5$) and entropy perbaryon $s$ = 8 $k_B$, and angular velocity is superimposed. In the early phase,the core collapses in a homologous manner. Then, it experiences a weak bouncedue to the gas pressure of free nucleons. Because the bounce is weak, the corecollapses eventually to a black hole. Subsequent evolution depends on initialangular velocity. When the rotation is not fast, a geometrically thin (butoptically thick) accretion disk is formed, and shock waves are formed in theinner part of the disk. For the moderately rotating case, the thin accretiondisk expands eventually to be a geometrically thick torus after sufficientaccumulation of the thermal energy generated at the shocks. Furthermore,convection occurs inside the torus. Neutrino luminosities vary violently withtime because of the convective motion. For the rapidly rotating case, bycontrast, a geometrically thick torus is formed soon after the black holeformation, and convective activity is weak due to the presence of epicyclicmode.

Formation of black hole and accretion disk in a massive high-entropy stellar core collapse