Speaker
Description
$^{12}C(\alpha,\gamma)^{16}O$ has been, and still is, one of the central topic in nuclear astrophysics.\
Reason for this is that stellar models are very sensitive to the ratio $^{12}C/^{16}O$ produced by the helium buring stage. Knowing the value of the $^{12}C(\alpha,\gamma)^{16}O$ S-factor at the energy of astrophysical interest ($E_0\sim$ 300 keV) to a precision better than 10\% would constrain our prediction on the isotopic aboundances and the fate of a star at the end of its evolution.\
The expected cross section at $E_0$ ($\sim 10^{-17}$ b) makes the direct measurement unfeasible and the complex $^{16}O$ energy levels structure require high precision measurement at higher energies to improve extrapolations of the S-factor.\
Recent developments have improved the ERNA separator installed at the Tandem laboratory of the University of Campania, Caserta that is now capable of measuring the $^{12}C(\alpha,\gamma)^{16}O$ cross section and its gamma emission angular distribution down to 1.0 MeV. \
In this contribution the commissioning of ERNA for the $^{12}C(\alpha,\gamma)^{16}O$ and perspective on the measurement campaign will be shown.
