THE WEAK s-PROCESS IN MASSIVE STARS AND ITS DEPENDENCE ON THE NEUTRON CAPTURE CROSS SECTIONS

By M. Pignatari, Roberto Gallino, M. Heil, Michael Wiescher, F. Käppeler, Falk Herwig, S. Bisterzo. 2010

233 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/54d6045337aef6f6d2f94d7ba31581121e687d93

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Citations in the corpus

NEUTRON-RICH CHROMIUM ISOTOPE ANOMALIES IN SUPERNOVA NANOPARTICLES (2010, background): “In SNII, neutron-rich isotopes are produced by neutron capture reactions during core C- and shell He-burning (Rauscher et al. 2002; The et al. 2007; Pignatari et al. 2010).”
The s process: Nuclear physics, stellar models, and observations (2010, methodology): “This has the important consequence that a particular MACS does not only determine the abundance of the respective isotope, but affects also the abundances of all heavier isotopes as well (Pignatari et al., 2010).”
CONVECTIVE–REACTIVE PROTON–12C COMBUSTION IN SAKURAI'S OBJECT (V4334 SAGITTARII) AND IMPLICATIONS FOR THE EVOLUTION AND YIELDS FROM THE FIRST GENERATIONS OF STARS (2010, background): “…be relevant in our case, since Rb, Sr, Y and Zr production is affected by the error of several low cross sections of isotopes in the mass region between Fe and Sr, acting like bottle-necks in the neutron capture flow (e.g., 62Ni, 68Zn, 74Ge and 78Se Pignatari et al. 2010, and reference therein).”
GALACTIC CHEMICAL EVOLUTION AND SOLAR s-PROCESS ABUNDANCES: DEPENDENCE ON THE 13C-POCKET STRUCTURE (2014, background): “Y–Zr, and in minor quantity up to Te–Xe (Pignatari et al. 2010, 2013). c Isotopes that receive an additional contribution from p process (Travaglio et al. 2011). d Overabundances with respect to solar (in percentage).”
NUGRID STELLAR DATA SET. I. STELLAR YIELDS FROM H TO BI FOR STARS WITH METALLICITIES Z = 0.02 and Z = 0.01 (2013, background): “36S has a different origin from the weak s process(e.g., Woosley et al. 2002; Mauersberger et al. 2004, and references therein), mainly via the production channel 35Cl(n,γ)36Cl(n,p)36S, where the initial 35Cl is the main seed (Mauersberger et al. 2004; Pignatari et al. 2010).”
Chemical evolution with rotating massive star yields - I. The solar neighbourhood and the s-process elements (2018, background): “…synthesis mainly during core He- and shell C-burning phases of massive stars (hereafter MS, M>≈ 10 M ) (Arnett & Thielemann 1985; Prantzos et al. 1990; Raiteri et al. 1991; Pignatari et al. 2010) with the reaction 22Ne(α, n)25Mg as the major neutron source (see Section 2.2 below for details).”
Nucleosynthesis in Stars and the Chemical Enrichment of Galaxies (2013, background): “Note that the weak s-process of massive stars may produce some Cu (Pignatari et al. 2010), but Cu production from hypernovae should be dominant.”
The Dawes Review 2: Nucleosynthesis and Stellar Yields of Low- and Intermediate-Mass Single Stars (2014, background): “It is the dominant neutron-producing reaction in the He and C-burning regions of massive stars (The et al. 2007; Heil et al. 2008; Pignatari et al. 2010) and the dominant neutron source in intermediate-mass AGB stars (Garćıa-Hernández et al. 2006; Karakas et al. 2012).”
SPECTRAL PROPERTIES OF COOL STARS: EXTENDED ABUNDANCE ANALYSIS OF 1,617 PLANET-SEARCH STARS (2016, background): “Yttrium The majority of yttrium nucleosynthesis happens in the weak s-process in massive stars; most of the remainder of Y nucleosynthesis taking place in the r-process (Busso et al. 1999; Pignatari et al. 2010; Maiorca et al. 2011).”
s-process production in rotating massive stars at solar and low metallicities (2015, methodology): “Since in He-burning conditions the amount of neutrons captured by light neutron poisons and not used for the s-process is lower compared to C-burning conditions, an overall increase of the s-process efficiency is obtained (see also Pignatari et al. 2010).”