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Abstract We present time-dependent nova outburst models with optically thick winds for 1. 2 and 1. 35\, M white dwarfs (WDs) with a mass-accretion rate of 5 10^-9\, M yr−1 and for a 1. 3\, M WD with 2 10^-9\, M yr−1. The X-ray flash occurs 11 d before the optical peak of the 1. 2\, M WD and 2. 5 d before the peak of the 1. 3\, M WD. The wind mass-loss rate of the 1. 2\, M WD (1. 3\, M WD) reaches a peak of 6. 4 10^-5\, M yr−1 (7. 4 10^-5\, M yr−1) at the epoch of the maximum photospheric expansion with the lowest photospheric temperature of log Tph (K) = 4. 33 (4. 35). The nuclear energy generated during the outburst is lost in the form of radiation (61% for the 1. 2\, M WD; 47% for the 1. 3\, M 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 tpeak and the expansion timescale τexp. With this relation, we are able to predict the time to optical maximum tpeak from the ignition model (at t = 0) without following a time-consuming nova wind evolution.
Kato et al. (Thu,) studied this question.