Mass and stability of rigidly rotating relativistic polytropes

Details Mass and stability of rigidly rotating relativistic polytropes Mass and stability of rigidly rotating relativistic polytropes

May 1974

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974stin...7512864v&link_type=abstract

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Physics

Stellar Mass, Stellar Rotation, Angular Momentum, Neutron Stars, Relativistic Theory, White Dwarf Stars

Scientific paper

The energy of a rigidly rotating star is written in the first and second post-Newtonian approximation. Conditions for equilibrium and stability are derived, as well as evolutionary paths for stars shedding angular momentum or mass. For polytropic index n 1, these analytic results agree with exact numerical results to within a few percent as long as the general relativity index (P/rho c squared)c 0.1 The energy methods is applied to low-mass white dwarfs, to semi-relativistic neutron stars, and to supermassive stars.

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