||We investigate the dependency of the inflow-wind structure of the hot accretion flow on the kinematic viscosity coefficient. Based on the previous studies on the accretion flow, we propose a model for the kinematic viscosity coefficient which would be null at the rotation axis and maximal at the equatorial plane. We compare our model with two other prescriptions from numerical simulations of the accretion flow. On this point, we solve the two-dimensional HD 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 prescriptions. On inspection, we find that in our model wind can extract a large amount of the angular momentum outward with regard to two other models presented here. The solutions obtained in this paper might be applicable for the numerical hydrodynamical simulations of the hot accretion flow.