Structure of the super-Eddington outflow and its impact on the cosmological scale

It is one of the biggest issues in black hole (BH) astrophysics how to precisely evaluate BH feedback its environments. Aiming at studying unique gas dynamics super-Eddington flow around supermassive (SMBH) seeds high redshift, we carried out axisymmetric two dimensional radiation hydrodynamic simulations by a nested simulation-box method. Here divide simulation box into inner zone $(2 - 3 \times 10^3) r_{\rm{Sch}}$ (with $r_{\rm Sch}$ being Schwarzschild radius) and outer $(2\times 10^{3} 3\times 10^6) r_{\rm{Sch}}$, with smooth connection physical quantities, such as density, velocity, energy. We start calculation injecting mass through boundary constant rate $\dot{M}_{\rm{inj}}=10^3L_{\rm{Edd}}/c^2$, where $L_{\rm{Edd}}$ Eddington luminosity $c$ speed light. A powerful outflow generated innermost region it propagates from zone. The outflows are characterized velocity 0.02$c$ (0.7$c$) density $10^{-17}$ ($10^{-19}$) g cm$^{-3}$ for near edge-on (face-on) direction. gradually accelerated travels accepting radiation-pressure force. final outermost $\dot{M}_{\rm{out}}\sim 0.3 \dot{M}_{\rm{inj}}$. By extrapolating structure further larger scale, find that momentum energy fluxes $r \sim 0.1$ pc $\sim 10-100 L_{\rm{Edd}}/c $ 0.1-10 L_{\rm{Edd}}$, respectively. Moreover, impacts highly anisotropic sense given towards face-on direction than These results indicate will more efficiently work on interstellar medium assumed cosmological simulations.