Explosive Nucleosynthesis in Near-Chandrasekhar-mass White Dwarf Models for Type Ia Supernovae: Dependence on Model Parameters

Abstract

We present two-dimensional hydrodynamics simulations of near-Chandrasekhar mass white dwarf (WD) models for Type Ia supernovae (SNe Ia) using the turbulent deflagration model with deflagrationdetonation transition (DDT). We perform a parameter survey for 41 models to study the effects of the initial central density (i.e., WD mass), metallicity, flame shape, DDT criteria, and turbulent flame formula for a much wider parameter space than earlier studies. The final isotopic abundances of 11 C to 91 Tc in these simulations are obtained by post-process nucleosynthesis calculations. The survey includes SNe Ia models with the central density from 5 × 10 8 g cm −3 to 5 × 10 9 g cm −3 (WD masses of 1.30 -1.38 M ⊙ ), metallicity from 0 to 5 Z ⊙ , C/O mass ratio from 0.3 -1.0 and ignition kernels including centered and off-centered ignition kernels. We present the yield tables of stable isotopes from 12 C to 70 Zn as well as the major radioactive isotopes for 33 models. Observational abundances of 55 Mn, 56 Fe, 57 Fe and 58 Ni obtained from the solar composition, well-observed SNe Ia and SN Ia remnants are used to constrain the explosion models and the supernova progenitor. The connection between the pure turbulent deflagration model and the subluminous SNe Iax is discussed. We find that dependencies of the nucleosynthesis yields on the metallicity and the central density (WD mass) are large. To fit these observational abundances and also for the application of galactic chemical evolution modeling, these dependencies on the metallicity and WD mass should be taken into account.

Smoothed particle inference analysis and abundance calculations of DEM L71, and comparison to SN explosion models

“… Note : S13: Seitenzahl et al (), L18: Leung & Nomoto (), M10: Maeda et al (), S16: Sukhbold et al (), N06: Nomoto et al (), M03: Maeda & Nomoto ().…”

A Nucleosynthetic Origin for the Southwestern Fe-rich Structure in Kepler’s Supernova Remnant

“…Future observations of Ti and Cr in 3C 397 will be interesting because the production of these elements in the n-NSE layer is very sensitive to the central density of the WD (e.g., Woosley 1997;Dave et al 2017;Leung & Nomoto 2018). 50 Ti and 52,54 Cr are produced at the deepest layers in near-M Ch explosions (see dashed green and solid purple curves in Figure 1).…”

The supernova remnant population of the Small Magellanic Cloud

“…Consequently, the SNR population of a galaxy collectively holds precious information on the dozen or hundreds of SNe which exploded recently within it. For instance, the ratio between the rates of SNe of each type (CC vs. type Ia) can in principle be recovered; the morphologies of individual SNRs can be linked to asymmetries either intrinsic to the explosion or coming from its surrounding ISM (Wongwathanarat et al 2013;Lopez 2014); and the abundances of newly-synthesised ejecta constrain details of both stellar evolution and explosion physics (Chieffi & Limongi 2017;Leung & Nomoto 2018).…”