On secular instabilities of rigidly rotating stars in general relativity. I - Theoretical formalism. II - Numerical results

Details On secular instabilities of rigidly rotating stars in general relativity. I - Theoretical formalism. II - Numerical results On secular instabilities of rigidly rotating stars in general relativity. I - Theoretical formalism. II - Numerical results

Oct 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979mnras.189..233c&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 189, Oct. 1979, p. 233-253, 255-272.

Computer Science

Numerical Analysis

35

Secular Variations, Stellar Models, Stellar Rotation, Angular Momentum, Astrophysics, Eigenvalues, Gravitational Fields, Long Term Effects, Neutron Stars, Numerical Analysis, Perturbation Theory, Rigidity, Stress Tensors, Tables (Data), White Dwarf Stars

Scientific paper

Equations are derived which give the e-folding times of the instabilities caused by an important class of nonaxisymmetric perturbations of the stars, while the stars are modeled as Maclaurin spheroids. It is reported that these instabilities cause the star's angular momentum to decrease and set upper limits to the angular frequency of stars with a given age. Using these equations it is shown that all incompressible, inviscid stars are secularly unstable to gravitational radiation reaction. It is found that when viscosity is introduced into the problem, it causes secular instabilities, however in some cases these two dissipative effects counterbalance each other and actually increase the secular stability of the star. In conclusion, it is noted that the e-folding times for solar density stars typically exceed the present lifetime of the universe, but for white dwarfs and neutron stars, these times can be of astrophysical interest.

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