  In order to precisely evaluate the impacts by super-Eddington accretors to
their environments, it is essential to assure a large enough simulation box and
long computational time to avoid any artefacts from numerical settings as much
as possible. In this paper, we carry out axisymmetric two-dimensional radiation
hydrodynamic simulations around a $10~M_\odot$ black hole in large simulation
boxes and study the large-scale outflow structure and radiation properties of
super-Eddington accretion flow for a variety of black hole accretion rates,
${\dot M}_{\rm BH} = (110 - 380) ~L_{\rm Edd}/c^2$. The Keplerian radius of the
inflow material, at which centrifugal force balances with gravitational force,
is fixed to 2430 Schwarzschild radii.We find that the mechanical luminosity
grows more rapidly than the radiation luminosity with an increase of ${\dot
M}_{\rm BH}$. When seen from a nearly face-on direction, especially, the
isotropic mechanical luminosity grows in proportion to ${\dot M}_{\rm
BH}^{2.7}$, while the total mechanical luminosity is proportional to ${\dot
M}_{\rm BH}^{1.7}$. The reason for the former is that the higher ${\dot M}_{\rm
BH}$ is, the more vertically inflated becomes the disk surface, which makes
radiation fields more confined in the region around the rotation axis, thereby
strongly accelerating outflowing gas. The outflow is classified into pure
outflow and failed outflow, depending whether outflowing gas can reach the
outer boundary of the simulation box or not. The fraction of the failed outflow
decreases with a decrease of ${\dot M}_{\rm BH}$. We analyze physical
quantities along each outflow trajectory, finding that the Bernoulli parameter
($Be$) is not a good indicator to discriminate pure and failed outflows, since
it is never constant because of continuous acceleration by radiation-pressure
force.Pure outflow can arise, even if $Be < 0$ at the launching point.
