Gravitational Collapse
Abstract
RECENTLY there has been renewed interest in the ultimate fate of the gravitational collapse of large masses. From the early work of Chandrasekhar^{1}, Oppenheimer and Volkoff^{2}, and the more recent work of others^{3}, it is clear that for a relativistic gas there is a critical spherical mass of M_{c} ~ 1 M_{solar}, where M_{solar} is the mass of the Sun. In any relativistic degenerate mass of M > M_{c}, no matter what radius it has, the gravitational field everywhere exceeds the outward force exerted by the pressure gradient. No static equilibrium configuration is possible, and hence the mass continuously collapses.
 Publication:

Nature
 Pub Date:
 December 1964
 DOI:
 10.1038/2041179a0
 Bibcode:
 1964Natur.204.1179H