The perturbations of a fully general relativistic and rapidly rotating neutron star. I - Equations of motion for the solid crust

Details The perturbations of a fully general relativistic and rapidly rotating neutron star. I - Equations of motion for the solid crust The perturbations of a fully general relativistic and rapidly rotating neutron star. I - Equations of motion for the solid crust

Feb 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992mnras.254..435p&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 254, Feb. 1, 1992, p. 435-452. Research supported by In

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11

Equations Of Motion, Neutron Stars, Relativistic Theory, Stellar Rotation, Stellar Structure, Gauge Theory, Helioseismology, Stellar Cores, Stellar Evolution, Stress Distribution, Supernovae

Scientific paper

The general relativistic theory of elasticity developed by Carter & Quintana is applied to the study of the solid crust of a fully general relativistic and rapidly rotating neutron star, the equations of motion of which are set up in the case of a uniform angular velocity. This unperturbed configuration is then perturbed in the most general way in order to write explicitly the general equations of motion of the solid part of the neutron star. No choice of gauge is made: keeping this gauge freedom as long as possible will simplify the comparison with other investigations, for which different choices of gauge were made; moreover, writing the equations of motion before choosing any gauge will help us to find the one by means of which they simplify as much as possible. The perturbed stress-energy tensor of elasticity is then studied together with the Lagrangian strain tensor and the constant volume strain tensor.

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