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Evolution in the spectrum of very slow novae PU Vul and V723 Cas during theirtransition from the optical maximum to the nebular phase is investigated usingthe method of disentangling the composite UV/optical spectra. Model SEDssuggested that a transient decrease in the WD luminosity, during the declinefrom the maximum, was caused by a negative beaming effect, when a neutral diskaround the WD was formed. When the disk disappeared, the luminosity increasedagain to values from the beginning of the outburst (in the case of V723 Cas,at/above the Eddington limit). This suggests the presence of a mechanismmaintaining a high energy output for a much longer time than it is predicted bythe current theories. Similarity of light curves, but enormous difference ofthe separation between the components of PU Vul and V723 Cas binaries suggestthat the mechanism is basically powered by the accretor.

Multiwavelength modeling the SED of very slow novae PU Vul and V723 Cas