Neutrino-driven wind simulations and nucleosynthesis of heavy elements

By A. Arcones, Friedrich-Karl Thielemann. 2012

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Neutrino-driven winds, which follow core-collapse supernova explosions, present a fascinating nuclear-astrophysics problem that requires an understanding of advanced astrophysics simulations, the properties of matter and neutrino interactions under extreme conditions, the structure and reactions of exotic nuclei, and comparisons with forefront astronomical observations. The neutrino-driven wind has attracted vast attention over the last 20 years as it was suggested as a candidate for the astrophysics site where half of the heavy elements are produced via the r-process. In this review, we summarize our present understanding of neutrino-driven winds from the dynamical and nucleosynthesis perspectives. Rapid progress has been made during recent years in understanding the wind with improved simulations and better micro physics. The current status of the fields is that hydrodynamical simulations do not reach the extreme conditions necessary for the r-process, and the proton or neutron richness of the wind remains to be investigated in more detail. However, nucleosynthesis studies and observations already point to neutrino-driven winds to explain the origin of lighter heavy elements, such as Sr, Y, Zr.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/09b98cdd3d173cb07f362f1548db712ece228c60

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Citations in the corpus

The Intermediate r-process in Core-collapse Supernovae Driven by the Magneto-rotational Instability (2016, background): “Tsujimoto & Nishimura (2015) showed that MR-SNe can explain the early growth of Eu in dwarf spheroidal galaxies for [Fe/H] −2 by assuming an event rate of about 0.5% of CC-SNe, while NSMs have problems to do so.”
THE r-PROCESS NUCLEOSYNTHESIS IN THE VARIOUS JET-LIKE EXPLOSIONS OF MAGNETOROTATIONAL CORE-COLLAPSE SUPERNOVAE (2015, background): “…aside from the long-standing problem of high entropies for a successful r-process, hydrodynamics simulations with detailed microphysics showed that the early neutron-rich ejecta of the winds immediately turn proton-rich (Fischer et al. 2010; Hüdepohl et al. 2010; Arcones & Thielemann 2013).”
NEUTRINO-DRIVEN WINDS IN THE AFTERMATH OF A NEUTRON STAR MERGER: NUCLEOSYNTHESIS AND ELECTROMAGNETIC TRANSIENTS (2015, background): “…required for a successful r-process (Arcones et al. 2007; Hüdepohl et al. 2010; Roberts et al. 2010; Fischer et al. 2010; Arcones & Montes 2011; Arcones & Thielemann 2013), though some rare supernovae may plausibly contribute (Fujimoto et al. 2006, 2008; Winteler et al. 2012; Mösta et al.…”
GALACTIC CHEMICAL EVOLUTION AND SOLAR s-PROCESS ABUNDANCES: DEPENDENCE ON THE 13C-POCKET STRUCTURE (2014, background): “In spite of promising theoretical improvements related to the explosive phases of massive stars and core collapse supernovae (Arcones & Thielemann 2013 and references therein), as well as recent spectroscopic investigations (Roederer 2012; Hansen et al. 2012, 2013), a full understanding of the…”
Europium production: neutron star mergers versus core-collapse supernovae (2013, background): “It seems now established that neutrino-driven winds from proto-neutron stars cannot be the main origin of the r-process elements beyondA ∼110 (Wanajo 2013; Arcones & Thielemann 2013).”