  We summarize results on the thermal and ionization structure of self-similar,
magnetically-driven, atomic disk winds heated by ambipolar diffusion. We
improve upon earlier work by Safier by considering (1) new MHD solutions
consistent with underlying cold keplerian disk equilibrium, (2) a more accurate
treatment of the micro-physics, and (3) predictions for spatially resolved
forbidden line emission (maps, long-slit spectra). The temperature plateau
$\simeq 10^4$ K found earlier is recovered, but ionization fractions are
revised downward by a factor of 10, due to previous omission of thermal speeds
in ion-neutral momentum-exchange rates. The physical origin of the temperature
plateau is outlined. Predictions are then compared with T~Tauri star
observations, with emphasis on the necessity of suitable beam convolution. Jet
widths and variations in line profiles with distance and line tracer are well
reproduced. However, predicted maximum velocities are too high, total densities
too low, and the low-velocity [OI] component is too weak. Denser, slower MHD
winds from warm disks might resolve these discrepancies.
