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 } _ { 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 the 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 .