  We present radiation-driven wind models for Luminous Blue Variables (LBVs)
and predict their mass-loss rates. We study the effects of lower masses and
modified abundances in comparison to the normal OB supergiants, and we find
that the main difference in mass loss is due to the lower masses of LBVs. In
addition, we find that the increase in helium abundance changes the mass-loss
properties by small amounts (up to about 0.2 dex in log Mdot), while CNO
processing is relatively unimportant for the mass-loss rate. A comparison
between our mass loss predictions and the observations is performed for four
relatively well-studied LBVs. The comparison shows that (i) the winds of LBVs
are driven by radiation pressure on spectral lines, (ii) the variable mass loss
behaviour of LBVs during their S Doradus-type variation cycles is explained by
changes in the line driving efficiency, notably due to the
recombination/ionisation of Fe IV/III and Fe III/II, and finally, (iii) the
winds of LBVs can be used to derive their masses, as exemplified by the case of
AG Car, for which we derive a present-day mass of 35 Msun.
