<span class="aps-inline-formula"><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mmultiscripts><mrow><mi mathvariant="normal">C</mi></mrow><mprescripts></mprescripts><mrow></mrow><mrow><mn>12</mn></mrow><mrow></mrow><mrow></mrow></mmultiscripts></mrow></math></span>(α,γ<span class="aps-inline-formula"><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msup><mrow><mo>)</mo></mrow><mrow><mn>16</mn></mrow></msup></mrow></math></span>O cross sections at stellar energies

J. M. L. Ouellet; H. C. Evans; H. W. Lee; J. R. Leslie; J. D. MacArthur; W. McLatchie; H.-B. Mak; P. Skensved; J. L. Whitton; X. Zhao; T. K. Alexander

doi:10.1103/PhysRevLett.69.1896

${}^{12}C$ (α,γ $)^{16}$ O cross sections at stellar energies

J. M. L. Ouellet, H. C. Evans, H. W. Lee, J. R. Leslie, J. D. MacArthur, W. McLatchie, H.-B. Mak, P. Skensved, J. L. Whitton, X. Zhao, and T. K. Alexander

Phys. Rev. Lett. 69, 1896 – Published 28 September 1992

Abstract

The excitation function of the ${}^{12}C$ (α,γ $)^{16}$ O reaction and the angular distribution of its γ rays were measured at nine energies ranging from $E_{c . m .}$ =1.37 to 2.98 MeV. These measurements allowed the separation of the E1 and E2 contributions and their extrapolation to the region of astrophysical interest. The analysis of the E1 cross sections with a three-level R-matrix method yields a prediction of $1_{- 1}^{+ 6}$ keV b for the S factor at $E_{c . m .}$ =0.3 MeV. The contribution of E2 transitions at the same energy is 40±7 keV b from a cluster-model analysis of the present data.