  We present time-dependent nova outburst models with optically thick winds for
a 1.2 and 1.35 $M_\odot$ white dwarfs (WDs) with a mass accretion rate of $5
\times 10^{-9}~M_\odot$ yr$^{-1}$ and for a 1.3 $M_\odot$ WD with $2 \times
10^{-9}~M_\odot$ yr$^{-1}$. The X-ray flash occurs 11 days before the optical
peak of the 1.2 $M_\odot$ WD and 2.5 days before the peak of the 1.3 $M_\odot$
WD. The wind mass loss rate of the 1.2 $M_\odot$ WD (1.3 $M_\odot$ WD) reaches
a peak of $6.4 \times 10^{-5}~M_\odot$ yr$^{-1}$ ($7.4 \times 10^{-5}~M_\odot$
yr$^{-1}$) at the epoch of the maximum photospheric expansion with the lowest
photospheric temperature of $\log T_{\rm ph}$ (K)=4.33 (4.35). The nuclear
energy generated during the outburst is lost in a form of radiation (61% for
the 1.2 $M_\odot$ WD; 47% for the 1.3 $M_\odot$ WD), gravitational energy of
ejecta (39%; 52%), and kinetic energy of the wind (0.28%; 0.29%). We found an
empirical relation for fast novae between the time to optical maximum from the
outburst $t_{\rm peak}$ and the expansion timescale $\tau_{\rm exp}$ at $t=0$.
With this relation, we are able to predict the time to optical maximum $t_{\rm
peak}$ from the ignition model (at $t=0$) without following a time-consuming
nova wind evolution.
