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The recognition that the metallicity of Type Ia supernova (SNIa) progenitorsmight bias their use for cosmological applications has led to an increasinginterest in its role on the shaping of SNIa light curves. We explore thesensitivity of the synthesized mass of 56Ni, M(56Ni), to the progenitormetallicity starting from Pre-Main Sequence models with masses M0 = 2 - 7 M_sunand metallicities Z = 1e-5 - 0.10. The interplay between convective mixing andcarbon burning during the simmering phase eventually rises the neutron excessand leads to a smaller 56Ni yield, but does not change substantially thedependence of M(56Ni) on Z. Uncertain attributes of the WD, like the centraldensity, have a minor effect on M(56Ni). Our main results are: 1) a sizableamount of 56 Ni is synthesized during incomplete Si-burning, which leads to astronger dependence of M(56Ni) on Z than obtained by assuming that 56Ni isproduced in material that burns fully to nuclear statistical equilibrium; 2) inone-dimensional delayed detonation simulations a composition dependence of thedeflagration-to-detonation transition density gives a non-linear relationshipbetween M(56Ni) and Z, and predicts a luminosity larger than previously thoughtat low metallicities (however, the progenitor metallicity alone cannot explainthe whole observational scatter of SNIa luminosities), and 3) an accuratemeasurement of the slope of the Hubble residuals vs metallicity for a largeenough data set of SNIa might give clues to the physics ofdeflagration-to-detonation transition in thermonuclear explosions.

Metallicity as a source of dispersion in the SNIa bolometric light curve luminosity-width relationship