New reaction rate for {sup 16}O(p,{gamma}){sup 17}F and its influence on the oxygen isotopic ratios in massive AGB stars

Journal Article · Tue Apr 15 04:00:00 EDT 2008 · Physical Review. C, Nuclear Physics

DOI:https://doi.org/10.1103/PHYSREVC.77.045802· OSTI ID:21189941

Iliadis, C ^[1]; Angulo, C ^[2]; Descouvemont, P ^[3]; Lugaro, M ^[4]; Mohr, P ^[5]

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1. Department of Physics and Astronomy, University of North Carolina, Chapel Hill, North Carolina 27599-3255 (United States)
2. Tractebel Engineering (SUEZ), Avenue Ariane 7, B-1200 Brussels (Belgium)
3. Physique Nucleaire Theorique et Physique Mathematique, CP229, Universite Libre de Bruxelles, B-1050 Brussels (Belgium)
4. Sterrenkundig Instituut, University of Utrecht, Postbus 80000, 3508 TA Utrecht (Netherlands)
5. Diakoniekrankenhaus Schwaebisch Hall, D-74523 Schwaebisch Hall (Germany)

The {sup 16}O(p,{gamma}){sup 17}F 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 {sup 16}O(p,{gamma}){sup 17}F 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.

• OSTI ID: 21189941
• Journal Information: Physical Review. C, Nuclear Physics, Journal Name: Physical Review. C, Nuclear Physics Journal Issue: 4 Vol. 77; ISSN 0556-2813; ISSN PRVCAN
• Country of Publication: United States
• Language: English

Related Subjects

73 NUCLEAR PHYSICS AND RADIATION PHYSICS
ASTROPHYSICS
ASYMPTOTIC SOLUTIONS
CROSS SECTIONS
FLUORINE 17
GIANT STARS
ISOTOPE RATIO
MASS
NUCLEAR REACTIONS
OXYGEN 16 TARGET
R MATRIX
REACTION KINETICS
STARS
STOPPING POWER
TEMPERATURE RANGE
TEMPERATURE RANGE OVER 4000 K
THERMONUCLEAR REACTIONS