The Schroedinger equation and cosmic bodies

Already in the very early days of the Schroedinger equation it was recognized that quantum theory was required to resolve problems of dense matter. Here a model star of non-relativistic neutrons which interact pairwise by the gravitational 1/r-potential is dealt with as a whole by quantum statistical mechanics. In an appropriate thermodynamic limit the free energy is given by Thomas-Fermi theory. The model neutron star undergoes a phase transition of first order if it cools down below a transition temperature. (Auth.)