56Ni, Explosive Nucleosynthesis, and SNe Ia Diversity

Abstract

The origin of the iron-group elements titanium to zinc in nature is understood to occur under explosive burning conditions in both Type Ia (thermonuclear) and Type II (core collapse) supernovae. In these dynamic environments, the most abundant product is found to be 56Ni (τ = 8.5 days) that decays through 56Co (τ = 111.5 days) to 56Fe. For the case of SNe Ia, the peak luminosities are proportional to the mass ejected in the form of 56Ni. It follows that the diversity of SNe Ia reflected in the range of peak luminosity provides a direct measure of the mass of 56Ni ejected. In this contribution, we identify and briefly discuss the factors that can influence the 56Ni mass and use both observations and theory to quantify their impact. We address specifically the variations in different stellar populations and possible distinctions with respect to SNe Ia progenitors.

6 pages, 2 figures

References in corpus (6)

• Rates and properties of type Ia supernovae as a function of mass and star-formation in their host galaxies
• The Dependence of Type Ia Supernova Luminosities on their Host Galaxies
• Double-detonation sub-Chandrasekhar supernovae: can minimum helium shell masses detonate the core?
• Detonations in Sub-Chandrasekhar Mass C+O White Dwarfs
• Distribution of ${}^{56}$Ni Yields of Type Ia Supernovae and its Implication for Progenitors
• Turbulence in a 3D deflagration model for type Ia SNe: II. Intermittency and the deflagration-to-detonation transition probability

Cited by in corpus (4)

• A reddening-free method to estimate the ${}^{56}$Ni mass of Type Ia supernovae
• Galactic Constraints on Supernova Progenitor Models
• The physics of the optical light curve in supernovae
• Three-body optical potentials in $(d,p)$ reactions and their influence on indirect study of stellar nucleosynthesis