The (54Fe+58Ni)/56Ni ratio as a second parameter for Type Ia supernova properties

Abstract

A variation of the relative content of (54Fe+58Ni) versus 56Ni may be responsible for the observed scatter of Type Ia Supernovae (SNe Ia) about a mean relation between their intrinsic brightness and the shape of their light curve. Synthetic light curves are computed of parametrised Chandrasekhar-mass explosion models of constant kinetic energy, where the ejecta are divided into an inner NSE zone, composed of (54Fe+58Ni) inside and 56Ni outside, an outer zone with Intermediate Mass Elements and a CO zone. Both the size of the NSE zone and the fraction of (54Fe+58Ni) v. 56Ni are varied systematically. Models with the same original NSE content but different (54Fe+58Ni)/56Ni ratios reach different peak brightness but have similar light curve shapes. Synthetic spectra indicate that the V-band decline rate is not affected by the (54Fe+58Ni)/56Ni ratio. While the 56Ni mass and the total NSE mass are the dominant parameters determining the peak luminosity and the shape of the light curve, respectively, a variation in the (54Fe+58Ni)/56Ni ratio, which may depend on the metallicity of the progenitor (Timmes, Brown & Truran 2003) is likely to account for a significant part of the observed scatter of local SNe Ia about the mean brightness--decline rate relation.