Rotating Polytropes in the Post-Newtonian Approximation

Abstract

It has been suggested by Fowler (1966) that rotation would make a star more stable, and Durney and Roxburgh (1967) have arrived at the same result, but so far the problem has not been treated without assuming that the star retains its shape (which it does not), and the post-Newtonian rotation terms have not been included. As a first step the equilibrium problem must be solved, and in this case the star is assumed to be a poly trope.