Abstract
The Thomas-Fermi model is used to calculate the equation of state (EOS) for nuclear as well as neutron matter. We apply the effective nucleon-nucleon interaction of Myers and Swiatecki which is velocity and density dependent. The calculations cover a wide density range of interest in heavy-ion collisions and astrophysics. We explore the thermodynamical behaviour of symmetric nuclear matter and neutron matter at finite temperature as it results from our EOS. As an illustration, the maximum stable mass of neutron star is calculated.