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Title:
New reaction rate for O16(p,γ)F17 and its influence on the oxygen isotopic ratios in massive AGB stars
Authors:
Iliadis, C.; Angulo, C.; Descouvemont, P.; Lugaro, M.; Mohr, P.
Affiliation:
AA(Department of Physics and Astronomy, University of North Carolina, Chapel Hill, North Carolina 27599-3255, USA; Triangle Universities Nuclear Laboratory, Durham, North Carolina 27708-0308, USA), AB(Tractebel Engineering (SUEZ), Avenue Ariane 7, B-1200 Brussels, Belgium), AC(Physique Nucléaire Théorique et Physique Mathématique, CP229, Université Libre de Bruxelles, B-1050 Brussels, Belgium), AD(Sterrenkundig Instituut, University of Utrecht, Postbus 80000, 3508 TA Utrecht, The Netherlands; Centre for Stellar and Planetary Astrophysics, School of Mathematical Sciences, Monash University, Victoria 3800, Australia), AE(Diakoniekrankenhaus Schwäbisch Hall, D-74523 Schwäbisch Hall, Germany)
Publication:
Physical Review C, vol. 77, Issue 4, id. 045802 (PhRvC Homepage)
Publication Date:
04/2008
Origin:
APS
PACS Keywords:
Stellar hydrogen burning, Nuclear reaction models and methods, Radiative capture, Radiative capture
DOI:
10.1103/PhysRevC.77.045802
Bibliographic Code:
2008PhRvC..77d5802I

Abstract

The O16(p,γ)F17 reaction rate is revisited with special emphasis on the stellar temperature range of T=60-100 MK, important for hot bottom burning in asymptotic giant branch (AGB) stars. We evaluate existing cross-section data that were obtained since 1958 and, if appropriate, correct published data for systematic errors that were not noticed previously, including the effects of coincidence summing and updated effective stopping powers. The data are interpreted by using two different models of nuclear reactions, that is, a potential model and R-matrix theory. A new astrophysical S factor and recommended thermonuclear reaction rates are presented. As a result of our work, the O16(p,γ)F17 reaction has now the most precisely known rate involving any target nucleus in the mass A⩾12 range, with reaction rate errors of about 7% over the entire temperature region of astrophysical interest (T=0.01-2.5 GK). The impact of the present improved reaction rate with its significantly reduced uncertainties on the hot bottom burning in AGB stars is discussed. In contrast to earlier results we find now that there is not clear evidence to date for any stellar grain origin from massive AGB stars.
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