Physics of nova outbursts: Theoretical models of classical nova outbursts with optically thick winds on 1.2 M⊙ and 1.3 M⊙ white dwarfs

We present time-dependent nova outburst models with optically thick winds for 1.2 and 1.35M(circle dot) white dwarfs (WDs) with a mass-accretion rate of 5x10(-9)M(circle dot) yr(-1) and for a 1.3M(circle dot) WD with 2x10(-9)M(circle dot) yr(-1). The X-ray flash occurs 11 d before the optical peak of the 1.2 circle dot WD and 2.5 d before the peak of the 1.3 circle dot WD. The wind mass-loss rate of the 1.2M(circle dot) WD (1.3M(circle dot) WD) reaches a peak of 6.4x10(-5)M(circle dot) yr(-1) (7.4x10(-5)M(circle dot) yr(-1)) at the epoch of the maximum photospheric expansion with the lowest photospheric temperature of log T-ph (K) = 4.33 (4.35). The nuclear energy generated during the outburst is lost in the form of radiation (61% for the 1.2M(circle dot) WD; 47% for the 1.3M(circle dot) 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(peak) and the expansion timescale tau(exp). With this relation, we are able to predict the time to optical maximum t(peak) from the ignition model (at t = 0) without following a time-consuming nova wind evolution.