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During the classical nova outburst, the radiation generated by the nuclearburning of hydrogen in the surface layer of a white dwarf (WD) is reprocessedby the outer material into different forms at softer energies, whichdistribution in the spectrum depends on the nova age. Using the method ofmultiwavelength modeling the SED we determined physical parameters of thestellar, nebular and dust component of radiation isolated from the spectrum ofthe classical nova V339 Del from day 35 to day 636 after its explosion. Thetransition 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 columndensity 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 $\sim2\times 10^{62}$ to $\sim 8.5\times 10^{60}$ cm$^{-3}$, was caused bystopping-down the mass-loss from the WD. The day 35 model SED indicated anoblate shape of the WD pseudophotosphere and the presence of the dust locatedin a slow equatorially concentrated outflow. The dust emission peaked aroundday 59. Its co-existence with the strong super-soft X-ray source in the day 100model SED constrained the presence of the disk-like outflow, where the dust canspend a long time. Both the models SED revealed a super-Eddington luminosity ofthe burning WD at a level of $1-2\times 10^{39}\,(d/4.5{\rm kpc})^2$ ergs$^{-1}$, lasting from $\sim$day 2 to at least day 100.

Multiwavelength modeling the SED of nova V339~Del: Stopping the wind and long-lasting super-Eddington luminosity with dust emission