A COMPARISON OF CALCULATED AND OBSERVED MONOCHROMATIC TYPE-IA SUPERNOVA LIGHT CURVES

The calculated monochromatic (B and V) light curves of a set of Type I a supernova models are compared with the observed monochromatic light curves of 13 Type Ia supernovae (SNIa). The set consists of 11 Type Ia supernova models including deflagrations, detonations, delayed detona tions, pulsating delayed detonations and tamped detonations. The theor etical light curves have been calculated using our recently developed light curve model. The model incorporates a detailed equation of state with an elaborate treatment of the ionization balance, an implicit gr ey LTE radiation transport scheme based on the moment equations, a tot al energy equation for the gas and the radiation field, expansion opac ities, and a Monte Carlo gamma-ray deposition scheme. To evolve the st ructure of the underlying explosion models homologous expansion is ass umed. We find that fast rising light curves (e.g., SN 1972E, SN 1981B and SN 1986G) can be reproduced best by delayed detonation models, and that slowly rising (t(max) greater than or similar 17 days) light cur ves (e.g., SN 1984A and SN 1990N) cannot be reproduced by standard det onation, deflagration or delayed detonation models. In order to obtain an acceptable agreement with observations for slowly rising light cur ves explosion models are required where the C/O white dwarf is surroun ded by an unburnt extended envelope of typically 0.2 to 0.4 M.. Our in terpretation of the light curves is also favoured from the expansion v elocities observed in the spectra of the slowly rising SNIa. Based on a comparison of theoretical light curves and observational data, the d istances of the parent galaxies have been determined. We show that SNe la allow for a measurement of the value of the Hubble constant provid ed individual fits are used and if they are located at distances large r than 15 Mpc, because only then they are in the ''Hubble'' flow. Taki ng this restriction into account a Hubble constant of H = 66 +/- 10 km /(secMpc) can be derived within a 2sigma error.