Type Ia supernovae: differences due to progenitors within delayed detonation explosions

At this moment, the use of SNIa for cosmology lies on the assumption that t he SNe at high redshifts are equal to the local ones. However, some observa tions indicate a correlation between light curve (LC) properties and the mo rphological type of the host galaxy. This could indicate a dependence with the age (mass/composition) of the underlying population. In this work we ha ve chosen the delayed detonation explosion model in CO Chandrasekhar mass W Ds to explore the dependence of the SNIa LC and nucleosynthesis with the in itial mass and composition of the WD progenitor. The progenitor influences the final SNIa via the mass of the CO core formed and the C/O ratio within it (1D explosion models). We have followed the evolution of stars with mass es between 1.5 and 8 M-circle dot and metallicity, Z=0, 10(-5), 0.001 and 0 .02, from the pre-main sequence to the TP-AGB phase. The differences obtain ed in the final C/O ratio within the explosive WD are smaller than 22%. Thi s results in a difference at maximum of 0.03 mag and of 0.1 mag when the br ightness-decline relation is applied.