Direct Collapse to Precursors of Supermassive Black Hole Seeds: Radiation-feedback-generated Outflows

Abstract We use high-resolution zoom-in cosmological simulations to model outflow triggered by radiation and thermal drivers around the central mass accumulation during direct collapse within dark matter (DM) halo. The maximal resolution is 1.3 × 10 −5 pc, no restrictions are put on geometry of inflow/outflow. considered prior formation supermassive black hole seed at a redshift z ∼ 15.9 can constitute either star (SMS) ∼10 5 M ⊙ surrounded growing accretion disk or self-gravitating disk. transfer modeled using ray-tracing algorithm. Due high rate ∼1 yr −1 determined DM halo, mildly supercritical, resulting in supercritical luminosity that has only limited effect rate, with duty cycle ∼0.9. observe fast development hot cavities, which quickly extend into polar funnels expand dense shells. Within funnels, winds, 3 km s , mass-loaded accreting gas. follow expanding shells when shell velocity remains substantially (∼5 times) above escape speed. ionization cones formed UV/X-ray completely ionize cavities. Extrapolating properties shows halo material outside will have difficulty stopping it. therefore conclude wind-driven break out parsec reach virial radius. Finally, anisotropic flow subparsec scales attenuate UV/soft X-rays H 2 . Hence, powerful outflows around, e.g., SMSs interesting observational corollaries.