In the past the global solar wind interaction with Venus has been treated principally with gas dynamic models. While this gas dynamic treatment has proven successful in modeling some of the global characteristics of the interaction, this model does not include the magnetic barrier in a self-consistent manner. This magnetic barrier is formed in the inner magnetosheath where it transfers solar wind momentum flux to the obstacle via magnetic pressure. In this study we examine the extent to which the gas dynamic fluid approximation describes the magnetic field in the dayside Venus magnetosheath by comparing with two gas dynamic models, one which matches the observed ionopause location and one which matches the bow shock location. We find that each model predicts the field profile reasonably well in the vicinity of the matched bow shock or ionopause but neither model provides an adequate model over the entire range from the ionopause to the bow shock. ¿ American Geophysical Union 1993