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We use high-resolution zoom-in cosmological simulations to model outflowtriggered by radiation and thermal drivers around the central mass accumulationduring direct collapse within the dark matter (DM) halo. The maximal resolutionis $1.3\times 10^{-5}$\,pc, and no restrictions are put on the geometry of theinflow/outflow. The central mass is considered {\it prior} to the formation ofthe supermassive black hole seed at a redshift of $z\sim 15.9$, and canconstitute either a supermassive star (SMS) of $\sim 10^5\,M_\odot$ surroundedby a growing accretion disk or a self-gravitating disk. The radiation transferis modeled using the ray-tracing algorithm. Due to the high accretion rate of$\sim 1\,M_\odot\,{\rm yr^{-1}}$ determined by the DM halo, accretion is mildlysupercritical, resulting in mildly super-critical luminosity which has only alimited effect on the accretion rate, with the duty cycle of $\sim 0.9$. Weobserve a fast development of hot cavities, which quickly extend into polarfunnels and expand dense shells. Within the funnels, fast winds, $\sim10^3\,{\rm km\,s^{-1}}$, are mass-loaded by the accreting gas. We follow theexpanding shells to $\sim 1$\,pc, when the shell velocity remainssubstantially, $\sim 5$ times, above the escape speed. The ionization conesformed by the central UV/X-ray completely ionize the cavities. Extrapolatingthe outflow properties shows that the halo material outside the shell will havedifficulty stopping it. We therefore conclude that the expanding wind-drivenshell will break out of the central parsec and will reach the halo virialradius. Finally, the anisotropic accretion flow on sub-parsec scales willattenuate the UV/soft X-rays on the H$_2$. Hence, the formation of funnels andpowerful outflows around, e.g., SMS, can have interesting observationalcorollaries.

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