Supernova Yield References - arsenal-popsynth/arsenal_gear GitHub Wiki
a quantity referenced often for nucleosynthesis in the innermost ejecta is the electron fraction,
- stars above 8
$\mathrm{M_\odot}$ explode as supernovae (SNe) with total kinetic energy$10^{51}$ ergs (McKee 1990) independent of SN type or metallicity - mass loss given by the stellar mass at central carbon exhaustion in the
evolutionary models minus the mass of the remnant (set to 1.4
$\text M_\odot$ ) - link: Leitherer et al. 1992
- yields for stable isotopes lighter than germanium ejected from stars of metallicities
$0, 10^{-4}, 10^{-2}, 0.1, \text{and } 1$ times the solar value (about 0.019 from Anders & Grevesse (1989)) - Each star is exploded using a piston to give a specified final kinetic energy at infinity, and the standard was taken to be
$1.2 \times 10^{51}$ ergs - For each star the piston was located at the outer edge of the iron core, which marks the outer extent of the last stage of convective silicon shell burning
- link: Woosley & Weaver 1995
- detailed yields for Chandrasekhar mass
$(\mathrm{1.38 M_\odot})$ models (Type Ia SNe) - 7 different models with explosion energies between 1.3 and 1.5
$\times 10^{51}$ ergs - link: Koichi et al. 1999
- Nucleosynthesis in Population III stars (metal free)
- used implicit hydrodynamics code KEPLER for all calculations
- grid of helium core masses from 65-130
$\text M_\odot$ in 5$\text M_\odot$ interval for detailed nucleosyntehsis - this range of helium core masses corresponds to
$\sim\text {140 - 260 M}_\odot$ stars - I couldn't find the raw data corresponding to explosion energies, but
$\text E_\text{expl}$ (kinetic energy at infinity) is given in Figure 1:
- link: Heger & Woosley 2002
- present nucleosynthesis yields as functions of mass, metallicity, and explosion energy
- take into account hypernovae (HNe), where the kinetic energy is
$\gtrapprox 10 \times 10^{51}$ ergs, as well as faint, lowe energy SNe - stars more massive than
$\sim 25 \text M_\odot$ form a black hole at the end of their evolution where non-rotating black holes are likely to have collapsed "quietly" ejecting a small amount of heavy elements, where stars with rotating black holes are likely to give rise to hypernovae - they suggest that the hypernova progenitors might form therapidly rotating cores by spiraling-in of a companion star in a binary system
- yields for a mass grid of
$\text{M = 13, 15, 18, 20, 25, 30, 40 M}_\odot$ , and a metallicity grid of$\text{Z = 0, 0.001, 0.004, 0.02}$ - the large Zn and Co abundances and the small Mn and Cr abundances observed in very metal-poor stars can be better explained by introducing HNe
- link: Nomoto et al. 2006
- explosion energy of Type II SNe around
$1.2 \text { B } \pm$ a factor of 2 (Bethe, named after Hans Bethe to represent$10^{51} \text {ergs}$ ) - largest difference for nucleosynthesis between
$1.2 \text{ B}$ and$2.4 \text{ B}$ explosions were iron group yields - note that a major shortcoming of Woover & Weasley 1995 was the omission of mass loss for massive stars - mass loss included in this work
- Masses included in the study were 12–33 solar masses in steps of 1
$\text M_\odot$ , plus stars of 35, 40, 45, 50, 55, 60, 70, 80, 100, and 120$\text M_\odot$ —32 stars altogether - link: Heger & Woosley 2007
- pre-supernova evolution of non-rotating stars of solar metallicity between masses of
$6.5-13.5 \text{ M}_\odot$ -
$\text{X = 0.711, Y = 0.274, Z = 0.015}$ - Hydrogen mass fraction, helium mass fraction, and metal mass fraction taken to be solar abundance, respectively (from Lodders 2003) - stars below 7 solar masses end their lives as carbon-oxygen white dwarfs, and
$7-9 \text{M}_\odot$ stars as oxygen-neon white dwarfs or electron capture SNe - link: Woosley & Heger 2015
- detailed yield tables, all at solar metallicity
- includes nucleosynthesis, light curves, explosion energies, and remnant masses
- grid of 200 pre-SN stars with masses from 9 to 120
$\text M_\odot$ - calculated using KEPLER code, very similar models to Woosley & Heger (2007, 2015), and Sukhbold & Woosley (2014)
- show "islands of explodability" where there is no mass of which below stars would explode as SNe and above collapse directly into BHs
- link: Sukhbold et al. 2016