  We analyze a 900-ks stacked Chandra/HETG spectrum of NGC 3783 in the context
of magnetically-driven accretion-disk wind models in an effort to provide tight
constraints on the global conditions of the underlying absorbers. Motivated by
the earlier measurements of its absorption measure distribution (AMD)
indicating X-ray-absorbing ionic columns that decrease slowly with decreasing
ionization parameter, we employ 2D magnetohydrodynamic (MHD) disk-wind models
to describe the global outflow. We compute its photoionization structure along
with the wind kinematic properties allowing us to further calculate in a
self-consistent fashion the shapes of the major X-ray absorption lines. With
the wind radial density profile determined by the AMD, the profiles of the
ensemble of the observed absorption features are determined by the two global
parameters of the MHD wind; i.e. disk inclination \theta_obs and wind density
normalization n_o. Considering the most significant absorption features in the
(~1.8A-20A) range, we show that the MHD-wind is best described by
n(r)~6.9e11(r/ro)^-1.15 [cm^-3] and \theta_obs=44deg. We argue that winds
launched by X-ray heating, radiation pressure or even MHD winds but with
steeper radial density profiles are strongly disfavored by data. Considering
the properties of Fe K band absorption features (i.e. Fe xxv and Fe xxvi),
while typically prominent in the AGN X-ray spectra, they appear to be weak in
NGC 3783. For the specific parameters of our model obtained by fitting the AMD
and the rest of absorption features, these features are found to be weak in
agreement with observation.
