  We propose a unified model for the nucleosynthesis of heavy (A > 57) elements
in stars. The neutron flux can be set to describe neutron capture in arbitrary
neutron flux. Our approach solves the coupled differential equations, that
describe the neutron capture and decays of 2696 nuclei, numerically without
truncating those to include only either capture or decay as traditionally
assumed in weak neutron flux (s process). As a result the synthesis of heavy
nuclei always evolves along a wide band in the valley of stable nuclei. The
observed abundances in the Solar system are reproduced reasonably already in
the simplest version of the model. The model predicts that the nucleosynthesis
in weak or modest neutron flux produces elements that are traditionally assumed
to result in the high neutron flux of supernovae explosions (r process).
