研究実績の概要 |
The goal of the 3rd year in our project was to calculate the advanced stage of direct collapse to a supermassive black hole seeds. We modeled the trapping of the continuum produced by the collapsing baryons, and formation of the core photosphere of the collapse. We have involved radiation transfer in the continuum. We solved the equation of radiative transfer in the Flux-Limited Diffusion (FLD) approximation, in tandem with the gravitational hydrodynamics of the collapse, including the radiation force in the Euler equation. Our results have, for the first time, demonstrated formation of the photosphere within the central 0.0001 pc of the 100 million solar mass dark matter halos. We have shown that the photons have been capable of escaping via preferred directions, developing convection. To demonstrate that the adiabatic approximation is inconsistent with the dynamics of the collapse, we compared our runs to adiabatic run, which cuts off the cooling. In summary, evolution of the adiabatic models diverges from that of the models involving a self-consistent radiation transfer. Finally, we have shown that the opaque core of the collapse is unstable, develops radiation-driven winds and can dissolve or its growth can be saturated. The current paradigm of a monotonic growth of the central core is not fulfilled with radiation transfer. Lastly, we find that the central core increases its spin with time, when the accretion flow with larger angular momentum arrives. This may lead to the formation of a self-gravitating disk with no central compact object.
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