2006ApJS..167...59H

We calculate many different nova light curves for a variety of white dwarf masses and chemical compositions, with the assumption that free-free emission from optically thin ejecta dominates the continuum flux. We show that all these light curves are homologous and a universal law can be derived by introducing a ``time scaling factor.'' The template light curve for the universal law has a slope of flux F∝t^–1.75 in the middle part (from ∼2 to ∼6 mag below the optical maximum), but it declines more steeply, F∝t^–3.5, in the later part (from ∼6 to ∼10 mag), where t is the time from the outburst in units of days. This break on the light curve is due to a quick decrease in the wind mass-loss rate. The nova evolutions are approximately scaled by the time of break. Once the time of break is observationally determined, we can derive the period of a UV burst phase, the duration of optically thick wind phase, and the turnoff date of hydrogen shell-burning. An empirical observational formula, t₃=(1.68±0.08) t₂+(1.9±1.5) days, is derived from the relation of F∝t^–1.75, where t₂and t₃are the times in days during which a nova decays by 2 and 3 mag from the optical maximum, respectively. We have applied our template light curve model to the three well-observed novae, V1500 Cyg, V1668 Cyg, and V1974 Cyg. Our theoretical light curves show excellent agreement with the optical y and infrared J, H, K light curves. The continuum UV 1455 Å light curves observed with IUE are well reproduced. The turn-on and turn-off of supersoft X-ray observed with ROSAT are also explained simultaneously by our model. The WD mass is estimated, from the light curve fitting, to be M_WD~1.15 M_☉for V1500 Cyg, M_WD~0.95 M_☉for V1668 Cyg, and M_WD~0.95-1.05 M_☉for V1974 Cyg, together with the appropriate chemical compositions of the ejecta.