Astrophysical S-factor of 14N( p, ?) 15O

By T. L. C. A. Formicola, G. Imbriani, H. Costantini. 2003

206 citations recorded by the source corpus.

We report on a new measurement of the 14N(p,γ) 15O capture cross section at Ep=140 to 400 keV using the 400 kV LUNA accelerator facility at the Laboratori Nazionali del Gran Sasso (LNGS). The uncer ...

Subfields: Atmospheric Science, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/dad621a1bfc8f540deaadae73836d32ebb63d4d5

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In Atmospheric Science

1. A. Serenelli
2. J. Bahcall
3. S. Basu
4. H. M. Antia
5. Martin Asplund
6. N. Grevesse

In Nuclear and High Energy Physics

1. S. Basu
2. H. M. Antia
3. A. Serenelli
4. C. Peña-Garay
5. Wick Haxton
6. J. Bahcall
7. Martin Asplund
8. E. Jenkins

Citations in the corpus

• Massive AGB models of low metallicity: the implications for the self-enrichment scenario in metal-poor globular clusters (2009, unknown): “14N(p,γ)15O (Formicola et al. 2004) 2.”
• Helioseismology and Solar Abundances (2007, background): “Recently, the cross section of the 14N(p, γ)15O reaction rate was reduced (Formicola et al. 2004).”
• SOLAR MODELS WITH ACCRETION. I. APPLICATION TO THE SOLAR ABUNDANCE PROBLEM (2011, background): “Since SFI a great deal of additional experimental and theoretical work has been done, e.g. 14N(p, γ)15O (Formicola et al. 2004; Imbriani et al. 2005; Runkle et al. 2005; Bemmerer et al. 2006b; 2 Lemut et al. 2006; Marta et al. 2008), 3He(4He, γ)7Be (Singh et al. 2004; Bemmerer et al. 2006a; Gyurky…”
• Yields of AGB and SAGB models with chemistry of low- and high-metallicity globular clusters (2013, unknown): “…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 al. 2004); 25Mg(p,γ)26Al…”
• New Solar Opacities, Abundances, Helioseismology, and Neutrino Fluxes (2004, methodology): “The model BS05(14N) is the same as the model BS04 except that in the newer model we use the recently measured value of S1,14 = 1.7±0.2 keV b for the low energy cross section factor of the 14N(p,γ)15O fusion reaction (Formicola et al. 2004).”
• Scaled solar tracks and isochrones in a large region of the Z-Y plane. II. From 2.5 to 20 solar masses (2009, methodology): “In our models, we tested the eff ct of measurements of the 14N(p, γ)15O reaction rate by the LUNA experiment (Formicola et al. 2004) and from the NACRE compilation (Angulo et al. 1999).”
• Ages and fundamental properties of Kepler exoplanet host stars from asteroseismology (2015, methodology): “…and those of Ferguson et al. (2005) for low temperatures, the NACRE compilation of nuclear reaction rates (Angulo et al. 1999) including the updated 14N(p, γ)15O reaction from Formicola et al. (2004), and the mixing-length theory of convection as described in Kippenhahn, Weigert & Weiss (2012).”