Metallicity Effects on
White Dwarf Supernovae


Astronomy research
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  White dwarf supernova:
     Remnant metallicities
     Colliding white dwarfs
     Merging white dwarfs
     Ignition conditions
     Metallicity effects
     Central density effects
     Detonation density effects
     Tracer particle burning
     Subsonic burning fronts
     Supersonic burning fronts
     W7 profiles
  Massive star supernova:
     Rotating progenitors
     3D evolution
     26Al & 60Fe
     44Ti, 60Co & 56Ni
     Yields of radionuclides
     Effects of 12C +12C
     SN 1987A light curve
     Constraints on Ni/Fe ratios
     An r-process
     Compact object IMF
     Pulsating white dwarfs
     Pop III with JWST
     Monte Carlo massive stars
     Neutrinos from pre-SN
     Pre-SN variations
     Monte Carlo white dwarfs
     SAGB stars
     Classical novae
     He shell convection
     Presolar grains
     He burn on neutron stars
     BBFH at 40 years
  Chemical Evolution:
     Hypatia catalog
     Zone models H to Zn
     Mixing ejecta
     γ-rays within 100 Mpc
  Thermodynamics & Networks
     Stellar EOS
     12C(α,γ)16O Rate
     Proton-rich NSE
     Reaction networks
     Bayesian reaction rates
  Verification Problems:
     Validating an astro code
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Contact: F.X.Timmes
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On Measuring The Metallicity Of A Type Ia Supernova's Progenitor (2016)
In Type Ia Supernovae (Sne Ia), the relative abundances of chemical elements are affected by the neutron excess in the composition of the progenitor white dwarf. Since these products leave signatures in the spectra near maximum light, spectral features may be used to constrain the composition of the progenitor. In this paper by Miles et al we calculate the nucleosynthetic yields for three SNe Ia simulations, assuming single degenerate, Chandrasekhar mass progenitors, for a wide range of progenitor metallicities, and calculate synthetic light curves and spectra to explore correlations between progenitor metallicity and the strength of spectral features. We use two 2D simulations of the deflagration-detonation-transition scenario with different 56Ni yields and the W7 simulation to control for differences between explosion models and total yields. While the overall yields of intermediate mass elements (16 < A ≤ 40) differ between the three cases, trends in the yields are similar. With increasing metallicity, 28Si yields remain nearly constant, 40Ca yields decline, and Ti and 54Fe yields increase. In the synthetic spectra, we identify two features at 30 days post explosion that appear to deepen with progenitor metallicity: a Ti feature around 4200 Å and a Fe feature around 5200 Å. In all three simulations, their pseudo equivalent widths show a systematic trend with progenitor metallicity. This suggests that these two features may allow differentiation among progenitor metallicities of observed SNe Ia and potentially help reduce the intrinsic Hubble scatter.

Si & Ti 30 days post-explosion
Si & Ti 30 days post-explosion
Si & Ti 30 days post-explosion
spectra of the DDT-high model for 5 metallicities at 10, 20, 30, and 40 days post-explosion
spectra at similar 56Ni yields
knock-out spectra for the DDT-low model with metallicity Z/Z=0.1
normalized maximum light NUV spectra

On Silicon Group Elements Ejected by Supernovae Type Ia (2014)
The electron fraction is set by the aboriginal composition of the white dwarf and the reactions that occur during the pre-explosive convective burning (see "Changes in Ye during the Simmering Phase" above). To date, determining the makeup of the white dwarf progenitor has relied on indirect proxies, such as the average metallicity of the host stellar population. In this paper by De et al we present analytical calculations supporting the idea that the electron fraction of the progenitor systematically influences the nucleosynthesis of silicon group ejecta in Type Ia supernovae. In particular, we suggest the abundances generated in quasi nuclear statistical equilibrium are preserved during the subsequent freezeout. This allows potential recovery of Ye at explosion from the abundances recovered from an observed spectra. We show that measurement of 28Si, 32S, 40Ca, and 54Fe abundances can be used to construct Ye in the silicon-rich regions of the supernovae. If these four abundances are determined exactly, they are sufficient to recover Ye to 6%. This is because these isotopes dominate the composition of silicon-rich material and iron-rich material in quasi nuclear statistical equilibrium. Analytical analysis shows that the 28Si abundance is insensitive to Ye, the 32S abundance has a nearly linear trend with Ye, and the 40Ca abundance has a nearly quadratic trend with Ye. We verify these trends with post-processing of 1D models and show that these trends are reflected in the model synthetic spectra.

QSE presevered during freezeout
Si-Group QSE & post-processeed
Fe-Group QSE & post-processeed
Global abundances vs Ye
Synthetic spectra of W7-like models

Changes in 56Ni from the expansion phase and 22Ne (2009)
Is there a systematic influence of 56Ni from 22Ne during the dynamical expansion phase of a white dwarf supernova? Some suprising answers are offered in Townsley et al. This effort also establishes a framework for exploring systematics effects in a grid of simulations.

different initial conditions
a Ye
changes in 56Ni

Changes in Ye during the Simmering Phase (2008)
Prior to the explosion of a carbon-oxygen white dwarf as a Type Ia supernova in the single-degenerate scenario there is a 100-1000 year simmering phase during which the 12C+12C reaction gradually heats the white dwarf. Chamulak et al and Piro & Bildsten show that weak reactions during this simmering phase set a maximum electron abundance Ye at the time of the explosion.

flows at ρ=109 g/cc
changes in Ye
light curve width changes

On Variations in the Peak Luminosity of Type Ia Supernovae (2003)
Why is there a variation in the peak luminosity of white dwarf supernovae? In this letter we explore how variations in the metallicity of the progenitor main sequence star gives rise to variations in the mass of 56Ni ejected. This effort has motivated several observational searches for the predicted effect.

birth metallicity vs 56Ni ejected
distant supernovae
metallicity scatter at any age