  Outflowing wind as one type of AGN feedback, which involves noncollimated
ionized winds prevalent in Seyfert-1 AGNs, impacts their host galaxy by
carrying kinetic energy outwards. However, the distance of the outflowing wind
is poorly constrained due to a lack of direct imaging observations, which
limits our understanding of their kinetic power and therefore makes the impact
on the local galactic environment unclear. One potential approach involves a
determination of the density of the ionized plasma, making it possible to
derive the distance using the ionization parameter {\xi}, which can be measured
based on the ionization state. Here, by applying a new time-dependent
photoionization model, tpho, in SPEX, we define a new approach, the tpho-delay
method, to calculate/predict a detectable density range for warm absorbers of
NGC 3783. The tpho model solves self-consistently the time-dependent ionic
concentrations, which enables us to study delayed states of the plasma in
detail. We show that it is crucial to model the non-equilibrium effects
accurately for the delayed phase, where the non-equilibrium and equilibrium
models diverge significantly. Finally, we calculate the crossing time to
consider the effect of the transverse motion of the outflow on the intrinsic
luminosity variation. It is expected that future spectroscopic observations
with more sensitive instruments will provide more accurate constraints on the
outflow density, and thereby on the feedback energetics.
