On the maximum mass of a neutron star
Abstract
The use of a variational method to determine an upper limit to the mass of the equilibrium configurations for a neutron star is discussed. For densities below the limit above which the interactions between neutrons change from attraction to repulsion, the HarrisonWheeler equation of state is applied. Above the limit value a variational procedure is used to determine the equation of state which provides the largest contribution to the mass; the only constraints are the constraints of causality and local stability of matter. The variational problem is defined with respect to three kinds of variations; these conditions indicate the appropriate Euler equations, transversality conditions, and ErdmannWeierstrass conditions. The requirement that the functional have negative curvature leads to the Laplace condition. Numerical integrations for some specific equations of state are examined.
 Publication:

Physics and Astrophysics of Neutron Stars and Black Holes
 Pub Date:
 1978
 Bibcode:
 1978pans.proc..583P
 Keywords:

 Critical Mass;
 Neutron Stars;
 Stellar Evolution;
 Stellar Mass;
 Black Holes (Astronomy);
 Calculus Of Variations;
 Equations Of State;
 Numerical Integration;
 Astrophysics