Cosmological direct-collapse black hole formation sites hostile for their growth

The direct collapse (DC) is a promising mechanism that provides massive seed black holes (BHs) with $\sim 10^{5}~M_{\odot}$ in the early universe. To study long-term accretion growth of DCBH thus formed, we perform cosmological radiation-hydrodynamics simulations, extending our previous work where investigated its formation stage. With high spatial resolution down below Bondi radius, show rate onto BH far Eddington value. Such slow mass partly because strong radiative feedback from accreting BH. Moreover, find has large velocity 100~{\rm km~s^{-1}}$ relative to gas after it falls into first galaxy, which substantially reduces rate. latter effect stems fact DCBHs form metal-free environments typically at 1~$kpc galaxy. accelerates as approaches galactic center due gravity. never damps that, and does not settle but continues wander around it. An analytic estimate predicts within 100$~pc necessary decelerate dynamical friction before $z=7$. Since metal enrichment $Z \sim 10^{-5} - 10^{-3}~Z_\odot$ expected such case, metal-poor preferable for subsequent rapid growth.