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