  We investigate the dependency of the inflow-wind structure of the hot
accretion flow on the kinematic viscosity coefficient. In this regard, we
propose a model for the kinematic viscosity coefficient to mimic the behavior
of the magnetorotational instability and would be maximal at the rotation axis.
Then, we compare our model with two other prescriptions from numerical
simulations of the accretion flow. We solve two-dimensional hydrodynamic
equations of hot accretion flows in the presence of the thermal conduction. The
self-similar approach is also adopted in the radial direction. We calculate the
properties of the inflow and the wind such as velocity, density, angular
momentum for three models of the kinematic viscosity prescription. On
inspection, we find that in the model we suggested wind is less efficient than
that in two other models to extract the angular momentum outward where the
self-similar solutions are applied. The solutions obtained in this paper might
be applicable to the hydrodynamical numerical simulations of the hot accretion
flow.
