On tidal phenomena in a strong gravitational field.
Abstract
A simple framework based on the concept of quadrupole tidal potential is presented for the calculation of tidal deformation of an extended test body in a gravitational field. This method is used to study the behavior of an initially faraway nonrotating spherical body that moves close to a Schwarzschild or an extreme Kerr black hole. In general, an extended body moving in an external gravitational field emits gravitational radiation due to its centerofmass motion, internal tidal deformation, and the coupling between the internal and centerofmass motions. Estimates are given of the amount of tidal radiation emitted by the body in the gravitational fields considered. The results reported are expected to be of importance in the dynamical evolution of a dense stellar system with a massive black hole in its center.
 Publication:

The Astrophysical Journal
 Pub Date:
 May 1975
 DOI:
 10.1086/153560
 Bibcode:
 1975ApJ...197..705M
 Keywords:

 Black Holes (Astronomy);
 Galactic Nuclei;
 Gravitational Fields;
 Star Clusters;
 Stellar Systems;
 Tides;
 Angular Momentum;
 Astronomical Models;
 Equations Of Motion;
 Galactic Evolution;
 Galactic Structure;
 Gravitational Waves;
 Potential Theory;
 Star Distribution;
 Astrophysics