Relativistic fluid disks in orbit around Kerr black holes.
Abstract
The general solution of the relativistic Euler equations for an ideal fluid is presented for the special case of the stationary, axisymmetric, purely azimuthal flow of isentropic fluid in an arbitrary stationary, axisymmetric gravitational field. In leaving the spacetime metric unspecified, the option of imposing Einstein's equations, and thus of taking the effects of selfgravitation into account is retained. As a particular example in which selfgravitation is ignored, the structure of those fluid disks around Kerr black holes which are characterized by constant angular momentum per unit inertial mass is studied. For each allowable equation of state, these solutions describe a twoparameter family of disks which can orbit a given Kerr black hole. Special attention is given to the influence of the black hole's angular momentum upon the structure of the given family of disks. One notable feature these disks exhibit is their pronounced thickness in the direction perpendicular to the equatorial plane of the Kerr field.
 Publication:

The Astrophysical Journal
 Pub Date:
 August 1976
 DOI:
 10.1086/154565
 Bibcode:
 1976ApJ...207..962F
 Keywords:

 Black Holes (Astronomy);
 Fluid Flow;
 Isentropic Processes;
 Relativistic Effects;
 Stellar Envelopes;
 Angular Momentum;
 Disks (Shapes);
 Euler Equations Of Motion;
 Flow Equations;
 Gravitational Fields;
 Newton Theory;
 Astrophysics