  I modelled the 14 \AA - 37 $\mu$m SED of the recurrent symbiotic nova RS Oph
during its supersoft source (SSS) phase and the following quiescent phase.
During the SSS phase, the model SEDs revealed the presence of a strong stellar
and nebular component of radiation in the spectrum. The former was emitted by
the burning WD at highly super-Eddington rate, while the latter represented a
fraction of its radiation reprocessed by the thermal nebula. During the
transition phase, both the components were decreasing and during quiescence the
SED satisfied radiation produced by a large, optically thick disk (R(disk) > 10
R(Sun)). The mass of the emitting material was (1.6 +/- 0.5) x 1E-4(d/1.6
kpc)**(5/2) M(Sun). The helium ash, deposited on the WD surface during the
whole burning period, was around of 8 x 1E-6(d/1.6kpc)**2 M(Sun), which yields
an average growing rate of the WD mass, dM(WD)/dt ~ 4 x 1E-7(d/1.6 kpc)**2
M(Sun)/yr. The mass accreted by the WD between outbursts, m(acc) ~ 1.26 x 1E-5
M(Sun), constrains the average accretion rate, dM(acc)/dt ~ 6.3 x 1E-7
M(Sun)/yr. If the wind from the giant is not sufficient to feed the WD at the
required rate, the accretion can be realized from the disk-like reservoir of
material around the WD. In this case the time between outbursts will extend,
with the next explosion beyond 2027. In the opposite case, the wind from the
giant has to be focused to the orbital plane to sustain the high accretion rate
at a few times 1E-7 M(Sun)/yr. Then the next explosion can occur even prior to
2027.
