  We study the dynamics of super-Eddington accretion flows by performing
two-dimensional radiation-hydrodynamic simulations. Compared with previous
works, in this paper we include the $T_{\theta\phi}$ component of the viscous
stress and consider various values of the viscous parameter $\alpha$. We find
that when $T_{\theta\phi}$ is included, the rotational speed of the
high-latitude flow decreases, while the density increases and decreases at the
high and low latitudes, respectively. We calculate the radial profiles of
inflow and outflow rates. We find that the inflow rate decreases inward,
following a power law form of $\dot{M}_{\rm in}\propto r^s$. The value of $s$
depends on the magnitude of $\alpha$ and is within the range of $\sim 0.4-1.0$.
Correspondingly, the radial profile of density becomes flatter compared with
the case of a constant $\dot{M}(r)$. We find that the density profile can be
described by $\rho(r)\propto r^{-p}$, and the value of $p$ is almost same for a
wide range of $\alpha$ ranging from $\alpha=0.1$ to $0.005$. The inward
decrease of inflow accretion rate is very similar to hot accretion flows, which
is attributed to the mass loss in outflows. To study the origin of outflow, we
analyze the convective stability of slim disk. We find that depending on the
value of $\alpha$, the flow is marginally stable (when $\alpha$ is small) or
unstable (when $\alpha$ is large). This is different from the case of
hydrodynamical hot accretion flow where radiation is dynamically unimportant
and the flow is always convectively unstable. We speculate that the reason for
the difference is because radiation can stabilize convection. The origin of
outflow is thus likely because of the joint function of convection and
radiation, but further investigation is required.
