  We study AGN emission line profiles combining an improved version of the
accretion disc-wind model of Murray & Chiang with the magneto-hydrodynamic
model of Emmering et al. (1992). Here we extend our previous work to consider
central objects with different masses and/or luminosities. We have compared the
dispersions in our model C IV linewidth distributions to observational upper
limit on that dispersion, considering both smooth and clumpy torus models.
Following Fine et al., we transform that scatter in the profile line-widths
into a constraint on the torus geometry and show how the half-opening angle of
the obscuring structure depends on the mass of the central object and the
accretion rate. We find that the results depend only mildly on the
dimensionless angular momentum, one of the two integrals of motion that
characterise the dynamics of the self-similar ideal MHD outflows
