论文标题
在巨大的云中，高质量恒星形成的辐射反馈，在原子冷却光环中具有H2分子
Radiative feedback for supermassive star formation in a massive cloud with H2 molecules in an atomic-cooling halo
论文作者
论文摘要
最新的三维形成的三维宇宙学模拟表明，超级质量恒星（SMS）可以在气云中形成，其中H $ _2 $冷却在激活原子冷却之前被动态加热抑制了（Wise等人，2019年），但它们停止了中部原蛋白蛋白质的以下生长。在这里，我们检查了在辐射反馈时，在这云中的原始核心上的积聚是否足够快，以产生SMS。我们对热崩溃的云进行了一维辐射流动力学模拟，其非平衡化学反应直接采用了Wise等人的云特性。 （2019）作为初始条件。我们发现，来自SMS的恒星Lyman-Werner（LW）辐射在气流的内部区域分离出H $ _2 $，增加了气温和热压，并暂时停止增生。但是，当较大尺度上的自我重力和内向RAM压力力推动气体向内推动时，这种负反馈就停止了。由于高密度，中央原始恒星无法扩展HII区域，并成长为$ \ gtrsim10^5 \，{{\ rm m} _ \ odot} $。我们的结果表明，SMSS的成功形成，并导致大量（$ \ sim10^5 \，{{\ rm m} _ \ odot} $）在云中残留的黑洞，但需要在两维模拟中确认。
Recent three-dimensional cosmological simulations of protogalaxy formation have suggested that supermassive stars (SMSs) can form in gas clouds in which H$_2$ cooling is suppressed by dynamical heating prior to the activation of atomic cooling (Wise et al. 2019), but they stopped short of the following growth of a central protostar. Here we examine whether accretion on the protostellar core in this cloud is sufficiently rapid, in the face of the radiation feedback, to produce a SMS. We perform one-dimensional radiation-hydrodynamical simulations of the hot collapsing cloud with non-equilibrium chemical reactions directly adopting the cloud properties from Wise et al. (2019) as an initial condition. We find that the stellar Lyman-Werner (LW) radiation from the SMS dissociates H$_2$ in the inner regions of the gas flow, increasing gas temperature and thermal pressure, and temporarily stopping the accretion. However, this negative feedback ceases when the self-gravity and inward ram pressure force on larger scales push the gas inward. The central protostar is unable to expand an HII region due to the high density, and grows to a mass of $\gtrsim10^5\,{{\rm M}_\odot}$. Our results suggests the successful formation of SMSs, and resulting massive ($\sim10^5\,{{\rm M}_\odot}$) remnant black holes in the clouds, but need to be confirmed in two- or three-dimensional simulations.
