  During the classical nova outburst, the radiation generated by the nuclear
burning of hydrogen in the surface layer of a white dwarf (WD) is reprocessed
by the outer material into different forms at softer energies, which
distribution in the spectrum depends on the nova age. Using the method of
multiwavelength modeling the SED we determined physical parameters of the
stellar, nebular and dust component of radiation isolated from the spectrum of
the classical nova V339 Del from day 35 to day 636 after its explosion. The
transition from the iron-curtain phase to the super-soft source phase (days 35
- 72), when the optical brightness dropped by 3-4 mag, the absorbing column
density fell by its circumstellar component from $\sim 1\times 10^{23}$ to
$\sim 1\times 10^{21}$ cm$^{-2}$, and the emission measure decreased from $\sim
2\times 10^{62}$ to $\sim 8.5\times 10^{60}$ cm$^{-3}$, was caused by
stopping-down the mass-loss from the WD. The day 35 model SED indicated an
oblate shape of the WD pseudophotosphere and the presence of the dust located
in a slow equatorially concentrated outflow. The dust emission peaked around
day 59. Its co-existence with the strong super-soft X-ray source in the day 100
model SED constrained the presence of the disk-like outflow, where the dust can
spend a long time. Both the models SED revealed a super-Eddington luminosity of
the burning WD at a level of $1-2\times 10^{39}\,(d/4.5{\rm kpc})^2$ erg
s$^{-1}$, lasting from $\sim$day 2 to at least day 100.
