  Aims. Our aim is to determine the distance of the UV outflow components from
the central source, their abundances and total column density, and the
mechanism responsible for their observed absorption variability.
  Methods. We studied the UV spectra acquired during the campaign as well as
from three previous epochs (2002-2010). Our main analysis tools are ionic
column-density extraction techniques and photoionization models (both
equilibrium and time-dependent models) based on the code Cloudy.
  Results. For component 1 (at -600 km/s) our findings include the following:
metallicity that is roughly twice solar; a simple model based on a fixed total
column-density absorber, reacting to changes in ionizing illumination that
matches the different ionic column densities derived from four spectroscopic
epochs spanning 13 years; and a distance of R=6+2.5-1.5 pc from the central
source. Component 2 (at -1430 km/s) has shallow troughs and is at a much larger
R. For component 3 (at -1880 km/s) our findings include: a similar metallicity
to component 1; a photoionization-based model can explain the major features of
its complicated absorption trough variability and an upper limit of 60 or 150
pc on R. This upper limit is consistent and complementary to the X-ray derived
lower limit of 12 or 31 pc for R. The total column density of the UV phase is
roughly 1% and 0.1% of the lower and upper ionization components of the warm
absorber, respectively.
  Conclusions. The NGC 7469 outflow shows super-solar metallicity similar to
the outflow in Mrk 279, carbon and nitrogen are twice and four times more
abundant than their solar values, respectively. Similar to the NGC 5548 case, a
simple model can explain the physical characteristics and the variability
observed in the outflow.
