The apsidal motion in binary stars. B.V.Vasiliev

The apsidal motion in binary stars. Abstract It is usually accepted to consider an apsidal motion in binary stars as a direct confirmation that a substance inside stars is not uniformly distributed. It is shown in this paper that the apsidal motion in binary systems observation data is in a good agreement with an existence of uniform plasma cores inside stars if they consist of hydrogen-deuterium-helium mixture. 1 An apsidal motion (an advance of periastron) of close binary stars is a result of their non-keplerian moving. It originates from a non-spherical form of stars. The last has been produced by a rotation of stars or their mutual tidal effects. The traditional approach to the estimation of a value of this effect needs to suppose some redistribution of mass inside stars to reach an accordance between the measured data and calculations. Usually it is necessary to assume that the density of a substance at the central region of a star is hundred times greater than a mean density of a star [1], [2]. On the face of it, the model of constant parameter [3],[4], where density inside a star core is constant, is in direct contradiction with the data of observation of an apsidal motion in close binary systems [5]. However, the traditional solution of the task about an apsidal motion is obtained for electrically non-charged matter. It is obvious that for electrically charged matter this solution must be reconsidered.