  Novae are the observational manifestations of thermonuclear runaways on the
surface of accreting white dwarfs (WDs). Although novae are an ubiquitous
phenomenon, their properties at low metallicity are not well understood. Using
the publicly-available stellar evolution code Modules for Experiments in
Stellar Astrophysics (MESA), we model the evolution of accreting carbon-oxygen
WDs and consider models which accrete matter with metallicity Z=0.02 or
$10^{-4}$. We consider both models without mixing and with matter enriched by
CO-elements assuming that mixing occurs in the process of accretion (with
mixing fraction 0.25). We present and contrast ignition mass, ejected mass,
recurrence period and maximum luminosity of novae for different WD masses and
accretion rates for these metallicities and mixing cases. We find that models
with Z = 0.02 have ignition masses and recurrence periods smaller than models
with low Z, while the ejected mass and maximum luminosity are larger. Retention
efficiency during novae outbursts decreases with increasing metallicity. In our
implementation, inclusion of mixing at the H/He interface reduces accreted
mass, ejected mass and recurrence period as compared to the no-mixing case,
while the maximum luminosity becomes larger. Retention efficiency is
significantly reduced, becoming negative in most of our models. For ease of
use, we provide a tabular summary of our results.
