  A quasar wind model is proposed to describe the spatial and velocity
structure of the broad line region. This model requires detailed
photoionization and magnetohydrodynamic simulation, as the broad line region it
too small for direct spatial resolution. The emission lines are Doppler
broadened, since the gas is moving at high velocity. The high velocity is
attained by the gas from a combination of radiative and magnetic driving
forces. Once this model is complete, the model predictions will be tested
against recent microlensing data in conjunction with diverse existing
observations.
