  We analyze the results of long-term observations of broad-line region (BLR)
in the Sy1 galaxy NGC 5548 and provide a critical comparison with the
predictions of a hydromagnetically-driven outflow model of Emmering, Blandford
and Shlosman. This model was used to generate a time series of CIV line
profiles that have responded to a time varying continuum. The model includes
cloud emission anisotropy, cloud obscuration, a CLOUDY-generated emissivity
function and a narrow-line component used to generate the line profiles, and is
driven with continuum input based on the monitoring campaigns of NGC 5548. The
line strengths, profiles and lags are compared with the observations. It
reproduces the basic features of CIV line variability in this AGN without
varying the model parameters. The best fit model provides the effective size,
the dominant geometry, the emissivity distribution and the 3D velocity field of
the CIV BLR and constrains the mass of the central BH. The inner part of the
wind appears to be responsible for the anisotropically emitted CIV line, while
its outer part remains dusty and molecular, thus having similar spectral
characteristics to a molecular torus, although its dynamics is fundamentally
different. In addition, our model predicts a differential response across the
CIV line profile, producing a red-side-first response in the mid-wings followed
by the blue mid-wing and by the line core. Based on the comparison of data and
model cross-correlation functions and 1D and 2D transfer functions, we find
that the rotating outflow model is compatible with observations of the BLR in
NGC 5548.
