tokens: axis due to the boundary conditions. The minimum value of v θ is also located around θ ∼ 43°. Moreover, the bottom right panel of Figure 1 presents the Mach numbers. We plot this figure to check the existence of the sonic point in the high-latitude region. As we can see, no sonic points exist in this region. The Mach number decreases from the equatorial plane to about 65°, where the radial velocity is zero. Then, it increases until θ = 30° and again decreases rapidly to the rotation axis. This behavior can be explained by the isothermal sound speed, c s = p / ρ . The profiles of the density and the total pressure in Figure 1 show that the density decreases rapidly from the equator to the pole while the pressure is almost constant in the range 0 θ 30°. Therefore, the Mach number declines in this range. Also, has a maximum value at θ = 43° and becomes null at both axes due to the boundary conditions there, i.e., v θ = 0. For both lines, the Mach numbers are less than unity, which clearly shows that there is no critical point at high latitudes. Figure 1. Angular profile of the physical variables at r = 10 r s . Top left panel: radial velocity in units of the light speed, c . The dashed line shows the location of v r = 0, which is about 65°. Top middle panel: latitudinal velocity in units of the Keplerian velocity, v 0 . Top right panel: angular velocity in units of the Keplerian angular velocity, Ω 0 . Bottom left panel: density in units of the density of the midplane at r 0 , i.e., ρ 0 . Bottom middle panel: radiation pressure in units of . Bottom right panel: Mach numbers. In the left panel of Figure 2 , we plot the two-dimensional distribution of the density overlaid with the streamlines of the flow. The results are shown for and the poloidal velocity is normalized by 0.1 c . It can be seen that the density tends to be larger around the midplane than around the polar axis. Moreover, the streamlines are directed toward the black hole at low latitudes with small magnitudes. At high latitudes, they are pointed outward and become outflow. For a high accretion rate, as in our present study, the outflow can be driven by the radiation pressure produced at inner radii. This strong radiation interacts with the gas particles and can push them away as a high-velocity outflow. This figure clearly shows the region of a high velocity field at high latitudes at r = 10 r s . As shown in the top left and top middle panels of Figure 1 , the poloidal velocity of the outflow reaches about ∼0.25 c . These results are fully consistent with the results obtained in Yang et al. ( 2014 , see their Figure 1) and Ohsuga et al. ( 2005 ), where the inflow is presented at low latitudes around the equatorial plane of the disk while the outflow is presented in the high-latitude regions. Figure 2. Two-dimensional distribution of the density (left) and the temperature (right) based on the self-similar solutions. Both panels are overlaid with the poloidal velocity. In the left
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