  Theoretical modelling of the evolution of classical and recurrent novae plays
an important role in studies of binary evolution, nucleosynthesis and accretion
physics. However, from a theoretical perspective the observed statistical
properties of novae remain poorly understood. In this paper, we have produced
model populations of novae using a hybrid binary population synthesis approach
for differing star formation histories (SFHs): a starburst case
(elliptical-like galaxies), a constant star formation rate case (spiral-like
galaxies) and a composite case (in line with the inferred SFH for M31). We
found that the nova rate at 10\;Gyr in an elliptical-like galaxy is $\sim
10-20$ times smaller than a spiral-like galaxy with the same mass. The majority
of novae in elliptical-like galaxies at the present epoch are characterized by
low mass white dwarfs (WDs), long decay times, relatively faint absolute
magnitudes and long recurrence periods. In contrast, the majority of novae in
spiral-like galaxies at 10\;Gyr have massive WDs, short decay times, are
relatively bright and have short recurrence periods. The mass loss time
distribution for novae in our M31-like galaxy is in agreement with
observational data for Andromeda. However, it is possible that we underestimate
the number of bright novae in our model. This may arise in part due to the
present uncertainties in the appropriate bolometric correction for novae.
