  Jets are a commonly observed phenomenon in post-asymptotic giant branch
(post-AGB) binaries. Due to the orbital motion of the binary, the jet causes
variable absorption in the Balmer profiles. In previous work, we have developed
spatio-kinematic and radiative transfer models to reproduce the observed Balmer
line variability and derive the spatio-kinematic structure of the jet and its
mass-loss rate. Here, we apply our jet model to five post-AGB binaries with
distinct H{\alpha} line variability and diverse orbital properties. Our models
fit the H{\alpha} line variations very well. We estimate jet mass-loss rates
between 10-8 Mdot yr-1 and 10-4 Mdot yr-1 , from which we deduce accretion
rates onto the companion between 10-7 Mdot yr-1 and 10-3 Mdot yr-1 . These
accretion rates are somewhat higher than can be comfortably explained with
reasonable sources of accretion, but we argue that the circumbinary disc in
these systems is most-likely the source feeding the accretion, although
accretion from the post-AGB star cannot be ruled out. The diversity of the
variability in the five objects is due to their wide ejection cones combined
with a range of viewing angles, rather than inherent differences between the
objects. The nature of the observations does not let us easily distinguish
which jet launching model (stellar jet, disc wind, or X-wind) should be
favoured. In conclusion, we show that our jet model includes the physical
parameters to successfully reproduce the H{\alpha} line variations and retrieve
the structure and mass-loss rates of the jet for all five objects that are
representative of the diverse sample of Galactic post-AGB binaries.
