Massive Stars in Quasi-Static Equlibrium.

Abstract

The binding energy properties of quasi-static solutions to the equations of general relativity for starlike condensations of 102 to 1O solar masses are presented. With increasing central temperature and decreasing radius, the binding energy first increases through positive values, passes through a maximum, and then decreases rapidly to large negative values. The central temperature at which maximum binding occurs follows the rough law T 3.4 X 1013C41o/M) K and the binding energy at this point is roughly 3.6 X 1O erg, nearly independent of mass.