  Observational evidence and many numerical simulations show the existence of
wind (i.e., uncollimated outflow) in accretion systems of the elliptical galaxy
center. One of the primary aims of this study is to investigate the solutions
of slowly rotating accretion flows around the supermassive black hole with
outflow. This paper presents two distinct physical regions: supersonic and
subsonic, that extend from the outer boundary to the black hole. In our
numerical solution, the outer boundary is chosen beyond the Bondi radius. Due
to strong gravity, we ignore outflow (i.e., $s = 0$) in the inner region
(within $\sim 10 r_s$). The radial velocity of the flow at the outer region is
significantly increased due to the presence of the outflow. Compared to
previous works, the one accretion mode - namely, slowly rotating case, which
corresponds to low accretion rates that have general wind output is carefully
described, and the effect of galaxy potential and the feedback effects by the
wind in this mode are taken into account. Since the power-law form of the mass
accretion rate is mathematically compatible with our equations, we consider a
radius-dependent mass accretion rate ($\dot{M}_{in} \propto r^s$), where $s$ is
a free parameter and shows the intensity of outflow. There is an unknown
mechanism for removing the mass, angular momentum, and energy by outflows in
this study. The effects of the outflow appear well on the outer edge of the
flow.
