  We solve the two-dimensional hydrodynamic equations of hot accretion flow in
the presence of the thermal conduction. The flow is assumed to be in
steady-state and axisymmetric, and self-similar approximation is adopted in the
radial direction. In this hydrodynamic study, we consider the viscous stress
tensor to mimic the effects of the magnetorotational instability for driving
angular momentum. We impose the physical boundary conditions at both the
rotation axis and the equatorial plane and obtain the solutions in the full $
r-\theta $ space. We have found that thermal conduction is indispensable term
for investigating the inflow-wind structure of the hot accretion flows with
very low mass accretion rates. One of the most interesting results here is that
the disc is convectively stable in hot accretion mode and in the presence of
the thermal conduction. Furthermore, the properties of wind and also its
driving mechanisms are studied. Our analytical results are consistent with
previous numerical simulations of hot accretion flow.
