  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(\alpha,\gamma)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(\alpha,\gamma)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.
