NEUTRON CROSS SECTIONS FOR NUCLEOSYNTHESIS STUDIES

By Z. Y. Bao, H. Beer, F. Käppeler, F. Voss, K. Wisshak, T. Rauscher. 2000

380 citations recorded by the source corpus.

Subfields: Nuclear and High Energy Physics, Radiation

View Paper: https://www.semanticscholar.org/paper/22a89c7df62cbaff9c407cc325813fbd9bf90ae9

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Citations in the corpus

THE JINA REACLIB DATABASE: ITS RECENT UPDATES AND IMPACT ON TYPE-I X-RAY BURSTS (2010, methodology): “Neutron capture reactions have also been extensively compiled (Allen et al. 1971; Bao & Käppeler 1987; Beer et al. 1992; Bao et al. 2000).”
The s process: Nuclear physics, stellar models, and observations (2010, methodology): “For easy access, the compilation of Bao et al. (2000) was published in electronic form via the KADoNiS project (http://www.kadonis.org) (Dillmann et al., 2005).”
GALACTIC CHEMICAL EVOLUTION AND SOLAR s-PROCESS ABUNDANCES: DEPENDENCE ON THE 13C-POCKET STRUCTURE (2014, methodology): “Travaglio et al. (2004) adopted the compilation by Bao et al. (2000), while we refer to KADoNiS (as well as few additional measurements listed above).”
Short-Lived Nuclei in the Early Solar System: A Low Mass Stellar Source? (2003, neutral): “The nuclear reaction rates involved are provided by extensive and sophisticated laboratory studies at the appropriate energies (Bao et al. 2000).”
ENDF/B-VII.1 Nuclear Data for Science and Technology: Cross Sections, Covariances, Fission Product Yields and Decay Data (2011, background): “Maxwellian-averaged cross sections (MACS) play an important role in power reactor developments and sprocess nucleosynthesis calculations [276].”
Is HE 0107–5240 A Primordial Star? The Characteristics of Extremely Metal-Poor Carbon-Rich Stars (2004, methodology): “When the – 19 – Bao et al. (2000) neutron-capture cross sections are adopted, the final oxygen abundance produced through these reactions varies from 4.0 × 10−3 to 0.022 as the abundance ratio of mixed-in 13C to 12C is varied from 13C/12C = 10−4 to 10−2.”
Rotational mixing in low-mass stars: II. Self-consistent models of Pop II RGB stars (2006, background): “By default the adopted rates are NACRE (Angulo et al. 1999) for charged particles, Bao et al. (2000) for neutron capture rates, Horiguchi et al. (1996) for experimental beta decay rates, and Caughlan & Fowler (1988) otherwise.”
s-Process Nucleosynthesis in Asymptotic Giant Branch Stars: A Test for Stellar Evolution (2002, background): “Rates for (n, ) reactions are updated to the latest estimates (Bao et al. 2000; Reifarth et al. 2001; Mutti et al. 2002).”
Isotopic Compositions of Strontium, Zirconium, Molybdenum, and Barium in Single Presolar SiC Grains and Asymptotic Giant Branch Stars (2003, methodology): “In Table 2 the half-lives of unstable isotopes involved in the s-path are given, together with theoretical estimates of cross sections from Bao et al. (2000) or, when not available, fromRauscher & Thielemann (2000).”
Nucleosynthesis in the Early Galaxy (2007, methodology): “Experimental Maxwellian average neutron capture cross sections and their temperature trends were taken from Bao et al. (2000) when available.”
Neutron-Capture Elements in the Early Galaxy (2008, background): “In particular, enhanced 23Na is produced in the thermal pulse by n-capture on the abundant 22Ne (in spite of its small capture cross-section, Bao et al. 2000).”