  We study the global solutions of slowly rotating accretion flows around the
supermassive black hole in the nucleus of an elliptical galaxy. The velocity of
accreted gas surrounding the black hole is initially subsonic and then falls
onto the black hole supersonically, so accretion flow must be transonic. We
numerically solve equations from the Bondi radius to near the black hole. The
focus of our discussion will be on the properties of slightly rotating
accretion flows in which radiative losses have been ignored. This study
discusses how outer boundary conditions (the temperature and specific angular
momentum at the outer boundary) influence accretion flow dynamics. We
investigate two physically discontinuous regimes: The Bondi-like type accretion
and the Disk-like type accretion. A Bondi-like accretion occurs when the
specific angular momentum at the Bondi radius $ \ell_{B} $ is smaller than the
specific angular momentum at the marginally stable orbit $ \ell_{ms} $. In
comparison, a Disk-like accretion occurs when the specific angular momentum at
the Bondi radius $ \ell_{B} $ is larger than the specific angular momentum of
the marginally stable orbit $ \ell_{ms} $. We also keep the assumption of
hydrostatic equilibrium and compare our results with the case in which it is
not considered. According to this study, considering the assumption of
hydrostatic equilibrium reduces the mass accretion rate. Additionally, we find
our solution for different ranges of the viscosity parameter $\alpha$. Finally,
we study the effect of galaxy potential on slowly rotating accretion flows.
