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Revision of the 15N(p, γ)16O reaction rate and oxygen abundance in H-burning zones
Istituto Nazionale di Fisica Nucleare (INFN), Sezione di Padova, via Marzolo 8, 35131 Padova, Italy; Dipartimento di Scienze della Terra, Università di Siena, 53100 Siena; and Centro di GeoTecnologie CGT, 52027 San Giovanni Valdarno, Italy .
Università degli Studi di Milano and INFN, Sezione di Milano, 20133 Milano, Italy.
Università degli Studi di Milano and INFN, Sezione di Milano, 20133 Milano, Italy.
Helmholtz–Zentrum Dresden–Rossendorf, Bautzner Landstr. 400, 01328 Dresden, Germany.
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2011 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 533, article id A66Article in journal (Refereed) Published
Abstract [en]

Context. The NO cycle takes place in the deepest layer of a H-burning core or shell, when the temperature exceeds T ≈ 30 × 106 K. The O depletion observed in some globular cluster giant stars, always associated with a Na enhancement, may be due to either a deep mixing during the red giant branch (RGB) phase of the star or to the pollution of the primordial gas by an early population of massive asymptotic giant branch (AGB) stars, whose chemical composition was modified by the hot bottom burning. In both cases, the NO cycle is responsible for the O depletion. Aims. The activation of this cycle depends on the rate of the 15N(p, γ)16O reaction. A precise evaluation of this reaction rate at temperatures as low as experienced in H-burning zones in stellar interiors is mandatory to understand the observed O abundances. Methods. We present a new measurement of the 15N(p, γ)16O reaction performed at LUNA covering for the first time the center of mass energy range 70-370 keV, which corresponds to stellar temperatures between 65 × 106 K and 780 × 106 K. This range includes the 15N(p, γ)16O Gamow-peak energy of explosive H-burning taking place in the external layer of a nova and the one of the hot bottom burning (HBB) nucleosynthesis occurring in massive AGB stars. Results. With the present data, we are also able to confirm the result of the previous R-matrix extrapolation. In particular, in the temperature range of astrophysical interest, the new rate is about a factor of 2 smaller than reported in the widely adopted compilation of reaction rates (NACRE or CF88) and the uncertainty is now reduced down to the 10% level. © 2011 ESO.

Place, publisher, year, edition, pages
EDP Sciences, 2011. Vol. 533, article id A66
Keywords [en]
Cataclysmic variables, Novae, Nuclear reactions, nucleosynthesis, abundances, Stars: AGB and post-AGB
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Identifiers
URN: urn:nbn:se:ltu:diva-7964DOI: 10.1051/0004-6361/201117475ISI: 000295168100066Scopus ID: 2-s2.0-80052209400Local ID: 6683ddad-3184-48a1-a381-1d2de0d54208OAI: oai:DiVA.org:ltu-7964DiVA, id: diva2:980854
Funder
German Research Foundation (DFG), BE 4100/2–1
Note

Funder: INFN; European Union (TARI RII3–CT–2004– 506222, AIM 025646 and SPIRIT 227012); Hungarian Scientific Research Fund(K68801)

Upprättat; 2011; 20141117 (albvom)

Available from: 2016-09-29 Created: 2016-09-29 Last updated: 2023-11-28Bibliographically approved

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