Nucleosynthesis and remnants in massive stars of solar metallicity

By Stan Woosley, Alexander Heger. 2007

573 citations recorded by the source corpus.

Abstract Hans Bethe contributed in many ways to our understanding of the supernovae that happen in massive stars, but, to this day, a first principles model of how the explosion is energized is lacking. Nevertheless, a quantitative theory of nucleosynthesis is possible. We present a survey of the nucleosynthesis that occurs in 32 stars of solar metallicity in the mass range 12– 120 M ⊙ . The most recent set of solar abundances, opacities, mass loss rates, and current estimates of nuclear reaction rates are employed. Restrictions on the mass cut and explosion energy of the supernovae based upon nucleosynthesis, measured neutron star masses, and light curves are discussed and applied. The nucleosynthetic results, when integrated over a Salpeter initial mass function (IMF), agree quite well with what is seen in the sun. We discuss in some detail the production of the long lived radioactivities, 26 Al and 60 Fe, and why recent model-based estimates of the ratio 60 Fe / 26 Al are overly large compared with what satellites have observed. A major source of the discrepancy is the uncertain nuclear cross sections for the creation and destruction of these unstable isotopes.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/c600e2f49307a421cf82648e40d108df77843ddd

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

The diversity of Type II supernova versus the similarity in their progenitors (2016, methodology): “…developed quantitative method of taking the ejecta stratification structure of a stellar model at the moment of explosion (e.g., the models of Woosley & Heger 2007), carrying out a detailed calculation of the energy deposition of gamma-rays/positrons by radioactive isotopes, and combining…”
THREE-DIMENSIONAL CORE-COLLAPSE SUPERNOVA SIMULATED USING A 15 M⊙ PROGENITOR (2015, methodology): “Initial conditions are taken from the 15 M pre-supernova progenitor of Woosley & Heger (2007).”
Unifying Type II Supernova Light Curves with Dense Circumstellar Material (2016, methodology): “We use non-rotating solar-metallicity RSG models from the stellar evolution code KEPLER (Weaver et al. 1978; Woosley & Heger 2007, 2015; Sukhbold & Woosley 2014; Sukhbold et al. 2016) with ZAMS masses in the range between 9M and 16.5M .”
Global comparison of core-collapse supernova simulations in spherical symmetry (2018, methodology): “We utilize the 20M (zero-age main sequence mass), solar metallicity, progenitor from [19] ‡.”
Non-Radial Instabilities and Progenitor Asphericities in Core-Collapse Supernovae (2014, methodology): “As we presently lack multi-D progenitor models at the onset of collapse, we impose artificial velocity and density perturbations on the progenitor model s15-2007 of Woosley & Heger (2007).”
The nebular spectra of SN 2012aw and constraints on stellar nucleosynthesis from oxygen emission lines (2013, methodology): “The Woosley & Heger (2007) final luminosities (from private communication with S. Woosley) are shown in Fig.”
What can be learned from a future supernova neutrino detection (2017, methodology): “[59] B. Müller, M. Viallet, A. Heger, and H.-T. Janka, “The Last Minutes of Oxygen Shell Burning in a Massive Star,” Astrophys.”
PTF12os and iPTF13bvn. Two stripped-envelope supernovae from low-mass progenitors in NGC 5806 (2016, methodology): “…of 12 M should be treated with some caution, since the models by Jerkstrand et al. (2015) are based on the singlestar nucleosynthesis models of Woosley & Heger (2007), and binary models can arrive at a He core with similar properties to our best-fitting model at the time of explosion for…”
SELF-SUSTAINED ASYMMETRY OF LEPTON-NUMBER EMISSION: A NEW PHENOMENON DURING THE SUPERNOVA SHOCK-ACCRETION PHASE IN THREE DIMENSIONS (2014, methodology): “We have performed 3D simulations for the evolution of the 11.2 M and 27 M progenitors of Woosley et al. (2002) and the 20 M model of Woosley & Heger (2007), using the high-density equation of state (EoS) of Lattimer & Swesty (1991) with a nuclear incompressibility of K = 220 MeV.”
BLACK HOLE FORMATION IN FAILING CORE-COLLAPSE SUPERNOVAE (2010, methodology): “ThesLC06B models are evolved with the W-R mass-loss rates of Langer (1989) that are similar to those used in thesWH07 set of Woosley & Heger (2007).”
A High-resolution Study of Presupernova Core Structure (2017, methodology): “Usually the settings on the network size are quite liberal, resulting in from 700 to 1,200 isotopes being carried in the early and late stages of evolution respectively (Woosley & Heger 2007).”
The overarching framework of core-collapse supernova explosions as revealed by 3D fornax simulations (2019, background): “M ) from Woosley & Heger (2007) and Woosley & Heger (2007) and did not include inelastic neutrino-electron or neutrino-nucleon scattering, nor velocity-dependent terms in the neutrino transport (see §2).”
NUCLEOSYNTHESIS AND EVOLUTION OF MASSIVE METAL-FREE STARS (2008, background): “…engine in these stars initially operates the same as in their modern counterparts (though fallback may differ), then present day constraints on nucleosynthesis, supernova light curves, and remnant masses (Weaver et al. 1978; Woosley & Heger 2007) limit our choices of explosion energy and mass cut.”
Type II-Plateau supernova radiation: dependences on progenitor and explosion properties (2013, methodology): “This comparison suggests that with theMESA STAR parameters employed to calculate the evolution of model m15Mdot, the final RSG structure and composition are qualitatively and quantitatively similar to theKEPLER model s15 (Woosley & Heger 2007).”
BRIGHT SUPERNOVAE FROM MAGNETAR BIRTH (2009, methodology): “The presupernova model adopted for our first study is a 4.37 M Wolf-Rayet star derived from the evolution of single 35 M main sequence star (Woosley & Heger 2007).”
SUB-CHANDRASEKHAR MASS MODELS FOR SUPERNOVAE (2010, background): “See Woosley & Heger (2007) for a summary.”