The equilibrium state of the dense electron-nuclear plasma in the self-gravitational field. The stellar mass distribution and stellar magnetic fields

Abstract

The equilibrium of dense plasma in a self-gravitation is considered. The obtained results radically distinguish from the point of view which is commonly accepted in the astrophysical society. It is important that all these results were obtained without any disputable speculative assumptions. They were obtained on the standard physical base by standard formal methods. The novelty of the obtained results is based on a rejection of the oversimplified ideal gas approximation which is usually accepted for a star interior description and on a taking into consideration the electron-nuclear plasma features. It was shown that there is the minimum for plasma energy at a density and a temperature which determines the equilibrium state of plasma in the self-gravitation at zero gradient of the general parameters of plasma. This effect plays an important role for astrophysics. It enables to explain the mechanism of the star magnetic field generation and to make a prediction for the spectrum of star masses with a quite satisfactory agreement for the observation data.