Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988phrvl..60.1475k&link_type=abstract
Physical Review Letters (ISSN 0031-9007), vol. 60, April 11, 1988, p. 1475-1478. Research supported by the W. K. Keck Foundation
Astronomy and Astrophysics
Astrophysics
68
Absorption Cross Sections, Carbon Monoxide, Nuclear Fusion, Reaction Kinetics, Stellar Evolution, Ground State, Helium
Scientific paper
Both the elemental abundance predicted from nucleosynthesis and the final evolutionary state of a massive star depend critically upon the rate of the reaction C-12(alpha, gamma)O-16. There is still considerable uncertainty in the value at stellar helium burning energies E(cm) of the astrophysical S factor, which removes most of the strong energy dependence of the reaction cross section due to Coulomb penetrability. Here, the E1 capture cross section for the reaction C-12(alpha, gamma)O-16 to the O-16 ground state is measured for E(cm) = 1.29-3.00 MeV. A three-level R-matrix analysis of E1 S factor leads to an allowed range for S(E1) at 300 keV of 0.00-14 MeV b. A model-dependent R-matrix analysis and a hybrid R-matrix analysis result in values of 0.14 and 0.08 MeV b, respectively, for S(E1)(300).
Barnes Charles A.
Chang Kao-Hao
Evans H. C.
Filippone B. W.
Kremer Richard M.
No associations
LandOfFree
Coincidence measurement of the (C-12)(alpha, gamma)(O-16) cross section at low energies does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Coincidence measurement of the (C-12)(alpha, gamma)(O-16) cross section at low energies, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Coincidence measurement of the (C-12)(alpha, gamma)(O-16) cross section at low energies will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-851141