The most important source of energy which powers the stars is hydrogen burning. For our Sun and for other low mass main sequence stars the hydrogen burning is realized mainly be the fusion reactions of the pp chains. In higher mass stars, on the other hand, the CNO cycles are the dominant processes of energy generation. The first CNO cycle is also important in the case of the Sun as its rate is directly related to the solar composition problem.
The slowest and thus most important reaction of the first CNO cycle is 14N(p,γ)15O. Its cross section was measured in many experiments, for example the ones carried out by the LUNA collaboration is Gran Sasso. Still, the reaction rate of 14N(p,γ)15O is not known with a precision required for astrophysical models. Further experimental works is therefore needed.
In this talk the status of the 14N(p,γ)15O reaction is reviewed in light of an ongoing experimental campaign at Atomki and a planned project at the upcoming LUNA-MV accelerator.
Institute for Nuclear Research (Atomki)