  The influence of the initial composition and structure of the exploding white
dwarf on the nucleosynthesis and structure of Type Ia Supernovae has been
studied.
  The progenitor structures are based on detailed stellar evolutionary tracks
for stars in the mass range between 1 to 9 $M_\odot$ using the state of the art
code FRANEC.
  The calculations of the thermonuclear explosions are based on a set of
delayed detonation models which give a good account of the optical and infrared
light curves and of the spectral evolution.
  Our code solves the hydrodynamical equations explicitly by the piecewise
parabolic method.
  Nuclear burning is taken into account using an extended network of 218
nuclei.
  In principle, our calculations allow the observed spectra and light curve to
be linked to the progenitor. Moreover, our study is relevant to estimate
potential evolution in the progenitor population at cosmological time scales.
