  Supernova rates (hypernova, type II, type Ib/c and type Ia) in a particular
galaxy depend on the metallicity (i.e. on the galaxy age), on the physics of
star formation and on the binary population. In order to study the time
evolution of the galactic supernova rates, we use our chemical evolutionary
model that accounts in detail for the evolution of single stars and binaries.
In particular, supernovae of type Ia are considered to arise from exploding
white dwarfs in interacting binaries and we adopt the two most plausible
physical models: the single degenerate model and the double degenerate model.
Comparison between theoretical prediction and observations of supernova rates
in different types of galaxies allows to put constraints on the population of
intermediate mass and massive close binaries. The temporal evolution of the
absolute galactic rates of different types of SNe (including the SN Ia rate) is
presented in such a way that the results can be directly implemented into a
galactic chemical evolutionary model. Particularly for SNIa the inclusion of
binary evolution leads to results considerably different from those in earlier
population synthesis approaches, in which binary evolution was not included in
detail.
