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Recent three-dimensional cosmological simulations of protogalaxy formationhave suggested that supermassive stars (SMSs) can form in gas clouds in whichH$_2$ cooling is suppressed by dynamical heating prior to the activation ofatomic cooling (Wise et al. 2019), but they stopped short of the followinggrowth of a central protostar. Here we examine whether accretion on theprotostellar core in this cloud is sufficiently rapid, in the face of theradiation feedback, to produce a SMS. We perform one-dimensionalradiation-hydrodynamical simulations of the hot collapsing cloud withnon-equilibrium chemical reactions directly adopting the cloud properties fromWise et al. (2019) as an initial condition. We find that the stellarLyman-Werner (LW) radiation from the SMS dissociates H$_2$ in the inner regionsof the gas flow, increasing gas temperature and thermal pressure, andtemporarily stopping the accretion. However, this negative feedback ceases whenthe self-gravity and inward ram pressure force on larger scales push the gasinward. The central protostar is unable to expand an HII region due to the highdensity, and grows to a mass of $\gtrsim10^5\,{{\rm M}_\odot}$. Our resultssuggests the successful formation of SMSs, and resulting massive($\sim10^5\,{{\rm M}_\odot}$) remnant black holes in the clouds, but need to beconfirmed in two- or three-dimensional simulations.

Radiative feedback for supermassive star formation in a massive cloud with H2 molecules in an atomic-cooling halo