We use a Monte Carlo technique together with a simple model for the di
stribution of dust in M31 to investigate the observability and spatial
distribution of classical novae in M31. By comparing our model positi
ons of novae to the observed positions, we conclude that most M31 nova
e come from the disk population, rather than from the bulge population
as has been thought. Our results indicate that the M31 bulge-to-disk
nova ratio is as low as, or lower than, the M31 bulge-to-disk mass rat
io.