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We know for sometime that nuclear forces and phenomena are the origin of
chemical elements in the Universe and are the fuel of the stars. To
quantitatively describe the processes involved we need more and better
nuclear data. These are being obtained either using direct measurements at
small acelerators and reactions at energies close to the ones involved in
stars, or through a select number of indirect methods with reactions at much
larger energies, which can then be translated in reaction rates at stellar
temperatures. I will briefly describe the most usual of the methods, with
examples from cases studied in my own group of young nuclear
astrophysicists: ion-ion fusion, Coulomb Dissociation, nuclear breakup,
transfer reactions, beta-delayed proton-decay, etc. Using IFIN-HH small
accelerators & an undergraound laboratory, or radioactive ion beams at
international laboratories.