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Tidal Stabilization of Rigidly Rotating, Fully Relativistic Neutron Stars

Kip S. Thorne
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Abstract

It is shown analytically that an external tidal gravitational field increases the secular stability of a fully general relativistic, rigidly rotating neutron star that is near marginal stability, protecting it against gravitational collapse. This stabilization is shown to result from the simple fact that the energy $δM(Q,R)$ required to raise a tide on such a star, divided by the square of the tide's quadrupole moment $Q$, is a decreasing function of the star's radius $R$, $(d/dR)[δM(Q,R)/Q^2]<0$ (where, as $R$ changes, the star's structure is changed in accord with the star's fundamental mode of radial oscillation). If $(d/dR)[δM(Q,R)/Q^2]$ were positive, the tidal coupling would destabilize the star. As an application, a rigidly rotating, marginally secularly stable neutron star in an inspiraling binary system will be protected against secular collapse, and against dynamical collapse, by tidal interaction with its companion. The ``local-asymptotic-rest-frame'' tools used in the analysis are somewhat unusual and may be powerful in other studies of neutron stars and black holes interacting with an external environment. As a byproduct of the analysis, in an appendix the influence of tidal interactions on mass-energy conservation is elucidated.

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BibTeXRIS

Kip S. Thorne. 1998-08-09. Tidal Stabilization of Rigidly Rotating, Fully Relativistic Neutron Stars. https://doi.org/10.1103/physrevd.58.124031

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