We have been developing a series of global coronal models directed at a better simulation of empirical coronal hole and streamer properties. In a previous study, a volumetric heat source was used to produce a thin current sheet above streamers and high solar wind speed in the coronal hole. This improved the preexisting coronal structure for coronal mass ejection simulations even when not using a polytropic energy equation. Here we report on the addition of a momentum source to the model with volumetric heating and thermal conduction. Most theoretical acceleration models in coronal holes are driven either by thermal pressure or waves (magnetosonic, Alfv¿n, and sonic waves). In the thermal pressure driven models an artificially high effective temperature is assumed. In the wave driven models the force is generally not big enough to accelerate the solar wind as quickly as observed. In the present model, in comparison to earlier calculations [Suess et al., 1996>, we reduce the heat source and add momentum. These changes appear to further improve the numerical simulation results in comparison to empirical properties. We have high solar wind speed in the hole without using unrealistic high plasma temperature. We also demonstrates that the deposition height of the momentum addition affects the mass flux. The model still predicts a slow-speed solar wind source in the streamer and high plasma &bgr; at the top of the streamer. ¿ 1998 American Geophysical Union