Our actual knowledge in stellar evolution and element synthesis in the Universe is at the heart of nuclear astrophysics field. The latter is interdisciplinary by excellence and it is enriched by the research performed in nuclear physics and astrophysics modeling as well as astronomic observations. Nuclear physics plays an important role to describe the energy production in stars and how they evolve. Thus, it is very important to improve our knowledge of nucleosynthesis processes occurring in the Universe and have a better knowledge of the nuclear properties (masses, decay half-life, density level, energy, spin-parity assignment and decay mode) of the nuclei involved in these processes. Usually the cross section of the nuclear reactions involved in stellar nucleosynthesis are very difficult to measure directly because of their very low value and/or the radioactive nature of the involved isotopes. Moreover, the cross sections for these reactions are strongly influenced by the resonances involved in the compound nucleus and the available nuclear models are not able to predict precisely the energy, spin-parity, total and decay widths of these resonances needed to calculate the reaction rates. To overcome these experimental difficulties, alternative methods such as transfer reactions and resonant scattering on thick target have been proposed