  We use a combined binary evolution code including dynamical effects to study
nova eruptions in a symbiotic system. Following the evolution, over $\sim10^5$
years, of multiple consecutive nova eruptions on the surface of a $1.25M_\odot$
white dwarf (WD) accretor, we present a comparison between simulations of two
types of systems. The first is the common, well known, cataclysmic variable
(CV) system in which a main sequence donor star transfers mass to its WD
companion via Roche-lobe overflow. The second is a detached, widely separated,
symbiotic system in which an asymptotic giant branch donor star transfers mass
to its WD companion via strong winds. For the latter we use the
Bondi-Hoyle-Lyttleton prescription along with orbital dynamics to calculate the
accretion rate. We use the combined stellar evolution code to follow the nova
eruptions of both simulations including changes in mass, accretion rate and
orbital features. We find that while the average accretion rate for the CV
remains fairly constant, the symbiotic system experiences distinct epochs of
high and low accretion rates. The examination of epochs for which the accretion
rates of both simulations are similar, shows that the evolutionary behaviors
are identical. We obtain that for a given WD mass, the rate that mass is
accreted ultimately determines the development, and that the stellar class of
the donor is of no significance to the development of novae. We discuss several
observed systems and find that our results are consistent with estimated
parameters of novae in widely separated symbiotic systems.
