On stars, their evolution and their stability

A mathematical criterion is derived for the stable existence of a star. Eddington's paradox and the related theory of white dwarf stars are explained. The upper limit is defined for the mass of stars which in the final stage may become a degenerated configuration. The degenerated core in the star develops with increasing density at constant temperature. Secular instability of rotating stars is derived on the basis of gravitational radiation in axially asymmetric oscillation modes. The principles of the mathematical theory of black holes are briefly explained. (M.D.)