Speaker
Description
The ${}^{12,13}\mathrm{C}(\mathrm{p},\gamma){}^{13,14}\mathrm{N}$ are the first reactions of the CNO cycle, active in both hydrostatic and explosive hydrogen burning. They contributes to the ${}^{12}\mathrm{C}$/${}^{13}\mathrm{C}$ isotopic ratio, observed in stellar atmosphere in meteoritic grains and in the interstellar medium. The ${}^{12}\mathrm{C}$/${}^{13}\mathrm{C}$ is a useful tool to study the mixing episodes and nucleosynthesis in Red Giant Branch (RGB) and Asymptotic Giant Branch (AGB) stars. A byproduct of the mixing events and nucleosynthesis taking place in Thermally pulsing AGB stars is the formation of the so called ${}^{13}\mathrm{C}$-pocket, which provides the neutron for s-process nucleosynthesis via the ${}^{13}\mathrm{C}(\alpha,\mathrm{n}){}^{16}\mathrm{O}$ reaction. Moreover the ${}^{12}\mathrm{C}(\mathrm{p},\gamma){}^{13}\mathrm{N}$ reaction is one of the main source of Solar CNO neutrinos, via the ${}^{13}\mathrm{N}$ decay.
Despite their important role in our understanding of stellar nucleosynthesis, up to recent years the ${}^{12,13}\mathrm{C}(\mathrm{p},\gamma){}^{13,14}\mathrm{N}$ reaction rates were poorly constrained by the few data available which are also affected by high uncertainty, with dramatic impact on our predictions for the the ${}^{12}\mathrm{C}$/${}^{13}\mathrm{C}$ isotopic ratio. In recent years, however, these two reactions have been the focus of renewed interest and of many experimental efforts. In the talk I will describe the complementary measurements recently performed at LUNA and at Felsenkeller underground laboratories in a wide energy region. In addition I will present results and I will compare them with previous literature and more recent data.
