Astrophysical Reaction Rate of 12C(α, γ)16O

By R. Kunz, M. Fey, M. Jaeger, A. Mayer, J. Hammer, G. Staudt, S. Harissopulos, T. Paradellis. 2002

207 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/cdcca0efb9a2aa4de905dc1517049eca9489967d

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Citations in the corpus

A new correction of stellar oscillation frequencies for near-surface effects (2014, methodology): “We used newer specific reaction rates for the reactions 14N(p, γ)15O (Imbriani et al. 2005) and 12C(α, γ)16O (Kunz et al. 2002).”
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): “…nuclear reactions, i.e., 14N(p,γ)15O, 3-α and 12C(α,γ)16O. Notice that the use of more recent rates (e.g., Imbriani et al. 2005; Fynbo et al. 2005; Kunz et al. 2002, respectively) would not change our results, where uncertainties related to physics processes and mixing still has a critical…”
Chemical evolution with rotating massive star yields - I. The solar neighbourhood and the s-process elements (2018, background): “It is possible that the use of the 12C(α, γ)16O rate from Kunz et al. (2002) in the case of LC2018 models, leads to somewhat larger production of C; the amount of mixing assumed in those models may also have a similar effect.”
The ACS Survey of Galactic Globular Clusters. II. Stellar Evolution Tracks, Isochrones, Luminosity Functions, and Synthetic Horizontal-Branch Models (2007, methodology): “Nuclear reaction rates were adopted from (Adelberger et al. 2002) with two exceptions: first, the 14N(p,γ)15O reaction (Imbriani et al. 2004) and second, the 12C(α,γ)16O reaction (Kunz et al. 2002).”
Evolution of Stars and Stellar Populations (2005, result): “According to [51], an uncertainty of the order of a factor of two is reasonable for this nuclear reaction rate (but see also the more recent analysis by [121]).”
The Adequacy of Stellar Evolution Models for the Interpretation of the Color-Magnitude Diagrams of Resolved Stellar Populations (2005, methodology): “Cassisi, Salaris & Irwin (2003) obtain Yp = 0.243±0.006 using the R parameter2 on GCs, and models with improved 12C(α, γ )16 O reaction rate (Kunz et al. 2002) and equation of state (Irwin 2005).”
MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA): PLANETS, OSCILLATIONS, ROTATION, AND MASSIVE STARS (2013, methodology): “Both models were evolved using the Kunz et al. (2002) rate for 12C(α, γ)16O.”
Constraints from Gravitational-wave Detections of Binary Black Hole Mergers on the 12C(α, γ)16O Rate (2020, methodology): “The STARLIB rate of Sallaska et al. (2013) is based on that of Kunz et al. (2002); however, STARLIB assumes that the rate probability density is log-normal, thus its median value is ´R RLow High (Equation (17) in Sallaska et al. 2013), where RLow and RHigh are from Kunz et al. (2002).”
Yields of AGB and SAGB models with chemistry of low- and high-metallicity globular clusters (2013, background): “…from the recommended values in the NACRE compilation (Angulo et al. 1999), with only the following exceptions: 3α (Fynbo et al. 2005); 12C(α,γ)16O (Kunz et al. 2002); 14N(p,γ)15O (Formicola et al. 2004); 22Ne(p,γ)23Na (Hale et al. 2002); 23Na(p,γ)24Mg (Hale et al. 2004); 23Na(p,α)20Ne (Hale et…”
MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA) (2010, unknown): “Signiﬁcant updates to the NACRE rates have been included for 14 N( p , γ ) 15 O (Imbriani et al. 2004), triple-α (Fynbo et al. 2005), 14 N( α, γ ) 18 F (G¨orres et al. 2000), and 12 C( α, γ ) 16 O (Kunz et al. 2002).”