Half-lives of neutron-rich nuclei and estimation of astrophysical r-processes duration

Microscopic model for the calculations of β-decay half-lives for neutron-rich nuclei is presented. Accuracy of the β-decay half-lives calculations is 40+50%. The dependence of r-process duration τA from temperature and neutron density is analysed. The minimal values of r-process duration under different conditions corresponding to the beginning of the heavy nuclei (A ≥ 240) synthesis are calculated. They restrict characteristic time in the dynamical model of the stellar explosion. So the nucleosynthesis problem must be treated selfconsistently using both nuclear models and hydrodynamical stellar calculations