Analysis of the Type IA Supernova SN 1994D

We present an analysis of the observed light curves and spectra of the Type Ia supernova SN 1994D in the galaxy NGC 4526. The sensitivity of theoretical light curves and spectra to the underlying hydrodynamical model is discussed. The calculations are consistent with respect to the explosion mechanism, the optical and infrared light curves, and the spectral evolution, leaving the description of the nuclear-burning front and the structure of the white dwarf as the only free parameters. The explosions are calculated using a one-dimensional Lagrangian code including a nuclear network (Khokhlov 1991). Subsequently, the light curves are constructed. Spectra are computed for several instants of time using the density, chemical, and luminosity structure resulting from the light- curve code. Our non-LTE (NLTE) code solves the relativistic radiation transport equations in a comoving frame consistently with the statistical equations and ionization due to γ-radiation for the most important elements (He, C, O, Ne, Na, Mg, Si, S, Ca, Fe). About 300,000 additional lines are included, assuming LTE-level populations and an equivalent-two- level approach for the source functions. We find that the classical two- level approach underestimates thermalization processes by several orders of magnitude. Besides models already discussed in previous papers, a new series of delayed detonations has been included with a ^56^Ni production ranging from ~0.2 up to 0.7 M_sun_ depending on the density at which the transition from a deflagration to a detonation occurs. The visual magnitude at maximum light M_V_ ranges from ~-18.4 to ~-19.5 mag. Only one model with M_V_ = - 19.39 mag shows good agreement with the observations of SN 1994D both for B, V, R, and I colors and the spectral evolution. The deflagration velocity is close to the laminar deflagration (ν = 0.03c_s_), and the transition from the deflagration to the detonation occurs at ρ_tr_ = 2 x 10^7^ g cm^-3^. The initial central density of the white dwarf is 2.7 x 10^9^ g cm^-3^, i.e., about 20% lower than in our delayed detonation models previously considered. The lower density may be understood in terms of a higher accretion rate on the progenitor. During the explosion, 0.6 M_sun_ of ^56^Ni are produced. The need to reduce Ti in the outer layers becomes evident from the spectral fits. This may be explained by small-scale density fluctuations during the explosion or by different primordial metallicity in the exploding white dwarf. The distance to SN 1994D is determined to 16.2 +/- 2 Mpc. The explosion took place between 1994 March 3 and 4.