The Astrophysical S-factor of the 12C(α,γ)16O Reaction at Solar Energies

Abstract

The astrophysical S-factor of the 4He-12C radiative capture is calculated in the potential model at the energy range 0.1-2.0 MeV. Radiative capture 12C(α,γ)16O is extremely relevant for the fate of massive stars and determines if the remnant of a supernova explosion becomes a black hole or a neutron star. Because this reaction occurs at low-energies the experimental measurements is very difficult and perhaps impossible. In this paper, radiative capture of the 12C(α,γ)16O reaction at very low-energies is taken as a case study. In comparison with other theoretical methods and available experimental data, excellent agreement is achieved for the astrophysical S-factor of this process.

6 pages, 1 figures, Submitted to Chinese Physics C

References in corpus (8)

• Quantum Monte Carlo calculations of neutron-alpha scattering
• Activation measurement of the 3He(alpha,gamma)7Be cross section at low energy
• Astrophysical S-factor of the 3He(alpha,gamma)7Be reaction measured at low energy via prompt and delayed gamma detection
• Microscopic calculation of the 3He(alpha,gamma)7Be and 3H(alpha,gamma)7Li capture cross sections using realistic interactions
• Evaluation of Modern 3He(alpha,gamma)7Be Data
• The 3He(alpha,gamma)7Be S-factor at solar energies: the prompt gamma experiment at LUNA
• Momentum-space calculation of proton-deuteron scattering including Coulomb and irreducible three-nucleon forces
• The n-n-alpha System in a Continuum Faddeev Formulation