Stability of Rotating Massive Stars in General Relativity

Details Stability of Rotating Massive Stars in General Relativity Stability of Rotating Massive Stars in General Relativity

Dec 1965

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1965natur.208.1304d&link_type=abstract

Nature, Volume 208, Issue 5017, pp. 1304-1305 (1965).

Physics

4

Scientific paper

THE suggestion by Hoyle and Fowler1 that stars with masses of 106-1010 Msolar may provide the energy for radio sources, and the subsequent discovery of quasars, has stimulated considerable interest in the structure of very massive stars2. Iben3, using a binding-energy argument, showed that within the framework of general relativity a spherical massive star becomes unstable long before it has contracted to the stage at which nuclear reactions become important. A similar conclusion was obtained by Chandrasekhar4, using a detailed stability analysis on the spherically symmetric relativistic equations and calculating the relaxation oscillations from a variational principle. Similar results have been obtained by Fowler5 using a virial theorem approach.

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