  Two types of nova evolutions can be realized in low mass white dwarfs of
~0.5-0.7 M_sun, i.e., an evolution with optically thick winds like in usual
classical novae, or an another type of evolution without them like in the
symbiotic nova PU Vul. The latter type is characterized by spectra of no
indication of strong winds as well as a long-lasted flat optical peak in its
light curve. We propose a transition from no-optically-thick-wind evolution to
usual evolution with optically thick winds as a new outburst model for slow
novae that show a relatively long-lasted multipeak phase followed by a wind
phase like in the slow novae V723 Cas, HR Del, and V5558 Sgr. We calculated
nova envelopes with one-dimensional approximation of the companion's effects
and found that when the companion star is deeply embedded in the extended nova
envelope, the structure of static envelope approaches that of the optically
thick wind solution. Thus, the transition from static to wind solution is
triggered by the effect of the companion. The transition occurs in a close
binary nova like V723 Cas, but is not triggered in a long period binary like PU
Vul. We reconfirm our previous results that the frictional energy deposition is
negligibly small in almost all of hydrogen/helium novae because of the low
envelope density at the orbit.
