2011MNRAS.410.2385T

We present 3D numerical simulations of the early evolution of long-duration gamma-ray bursts in the collapsar scenario. Starting from the core collapse of a realistic progenitor model, we follow the formation and evolution of a central black hole and centrifugally balanced disc. The dense, hot accretion disc produces freely escaping neutrinos and is hydrodynamically unstable to clumping and to forming non-axisymmetric (m = 1, 2) modes. We show that these spiral structures, which form on dynamical time-scales, can efficiently transfer angular momentum outwards and can drive the high required accretion rates ( ≥ 0.1-1 M_☉/s) for producing a jet. We utilize the smoothed particle hydrodynamics code, GADGET-2, modified to implement relevant microphysics, such as cooling by neutrinos, a plausible treatment approximating the central object and relativistic effects. Finally, we discuss implications of this scenario as a source of energy to produce relativistically beamed γ-ray jets.