Proton-induced Thermonuclear Reaction Rates for A = 20–40 Nuclei

By C. Iliadis, J. DAuria, S. Starrfield, W. J. Thompson, Michael Wiescher. 2001

181 citations recorded by the source corpus.

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

View Paper: https://www.semanticscholar.org/paper/1c51cf54bb9eb1eea03029b5480bd2304c48891f

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Citations in the corpus

The Nucleosynthesis of 26Al and 60Fe in Solar Metallicity Stars Extending in Mass from 11 to 120 M☉: The Hydrostatic and Explosive Contributions (2006, background): “Although the uncertainty quoted for this process (e.g., Iliadis et al. 2001) is of the order of a factor of 2 in the temperature range 0:02 T9 0:2, we preferred to explore the general theoretical dependence of the 26Al (ejected by the wind) on the MG25PG cross section in a range of values wider…”
Fast rotating massive stars and the origin of the abundance patterns in galactic globular clusters (2006, methodology): “The three other cases include the updates of Iliadis et al. (2001) and Hale et al. (2002, 2004) for the reactions involved in the NeNa and MgAl chains but with different options (see Table 2).”
Nucleosynthesis in Massive Stars with Improved Nuclear and Stellar Physics (2001, methodology): “Our standard set of light element reaction rates begins with Caughlan & Fowler (1988) as updated by Hoffman et al. (2001) and Iliadis et al. (2001).”
STARLIB: A NEXT-GENERATION REACTION-RATE LIBRARY FOR NUCLEAR ASTROPHYSICS (2011, methodology): “Setoodehnia et al. (2010) reaffirms the existence of a level predicted to be 3+ (Ex = 4693(5) keV), previously observed in Bardayan et al. (2007), and measured the energy of the potential 2+ level (Ex = 4814(3) keV) for the first time, decreasing the uncertainty in the energy estimated using the IMM”
NUGRID STELLAR DATA SET. I. STELLAR YIELDS FROM H TO BI FOR STARS WITH METALLICITIES Z = 0.02 and Z = 0.01 (2013, unknown): “0, and Basel REACLIB, revision 20090121 Cyburt 2011; Rauscher & Thielemann 2000, respectively), KADoNIS (Dillmann et al. 2006), NACRE (Angulo et al. 1999), CF88 (Caughlan & Fowler 1988), (Iliadis et al. 2001).”
The Effects of Thermonuclear Reaction-Rate Variations on Nova Nucleosynthesis: A Sensitivity Study (2002, methodology): “This point has been discussed in more detail by Iliadis et al. (2001).”
The Dawes Review 2: Nucleosynthesis and Stellar Yields of Low- and Intermediate-Mass Single Stars (2014, background): “The rate of 23Na destruction is important for determining Na yields (e.g., Iliadis et al. 2001; Izzard et al. 2007).”
The s process: Nuclear physics, stellar models, and observations (2010, background): “…at the various s-process sites and for further stellar evolution see the compiled data of the NACRE collaboration (Angulo et al., 1999) and of Iliadis et al. (2001) as well as recent work on 12C (Assunção et al., 2006; Plag et al., 2005) and on the two major neutron source reactions 13C(α,…”
THE JINA REACLIB DATABASE: ITS RECENT UPDATES AND IMPACT ON TYPE-I X-RAY BURSTS (2010, methodology): “Many of the experiment-based reaction rates were taken from the compilations of the NACRE collaboration (Angulo et al. 1999) and from Iliadis et al. (2001) for stable and unstable nuclei respectively.”
Thermohaline instability and rotation-induced mixing - III. Grid of stellar models and asymptotic asteroseismic quantities from the pre-main sequence up to the AGB for low- and intermediate-mass stars of various metallicities (2012, background): “For proton captures on elements higher then Ne, we follow rates from Iliadis et al. (2001) or otherwise Bao et al. (2000).”
Thermohaline instability and rotation-induced mixing I. Low- and intermediate-mass solar metallicity stars up to the end of the AGB (2010, unknown): “…with the exception of : 14C(p,γ)15N (Wiescher et al. 1990); 14C(p,n)14N (Koehler & O’brien 1989); 14C(p,α)11B (Caughlan & Fowler 1988); 14N(p,γ)15O (Mukhamedzhanov et al. 2003); 21Ne(p,γ)22Na, 22Na(p,γ)23Na, 23Na(p,α)20Ne, and 23Na(p,γ)24Mg (Iliadis et al. 2001);22Ne(p,γ)23Na (Hale et al. 2002).”
Updated stellar yields from asymptotic giant branch models (2009, background): “The most important changes are the 21Ne(p, γ)22Na rate from Iliadis et al. (2001), the 22Ne(p, γ)23Na rate from Hale et al. (2002), and the 23Na(p, γ)24Mg and 23Na(p, α)20Ne rates from Hale et al. (2004).”