Using magnetospheric MHD codes for space weather prediction has many advantages over other techniques including the specification of the entire magnetospheric state instead of some subsection, such as the ionospheric electric potential pattern. Time-dependent MHD simulations are computationally expensive and therefore nonfeasible to continuously run in real time. This study focuses on determining whether a quasi steady state magnetospheric configuration, determined by an MHD code, can be used as a prediction for the true state of the magnetosphere during relatively steady interplanetary magnetic field (IMF) intervals. To determine the feasibility of this, the University of Michigan MHD code was run to a nearly steady solution using the average IMF By and Bx and solar wind conditions observed on March 19--20, 1999. The IMF Bz was set to nearly the minimum observed during this period. Ground-based magnetograms were simulated using the model output, which were then compared with the actual magnetograms for the given stations, using the root-mean-square (RMS) difference to determine the error. The RMS differences were compared to the RMS variation of the data. Different ionospheric conductance models were used to investigate possible sources of error. The model results within the polar cap and at lower latitudes showed that the model was reproducing the global structure of the region 1 currents accurately. It is further noted that the RMS differences leave room for significant improvement in the specification. ¿ 2001 American Geophysical Union