Solutions of the equations of stellar hydrodynamics for Eddington systems
Abstract
The equations of stellar hydrodynamics for Eddington's stellar systems with separable potentials are written in coordinates based on principal velocity surfaces. When these surfaces are elliptic cylindrical or spheroidal, it is shown that the equations can be solved by Green's function methods to give the components of the stress tensor needed to support the system. Thus, if the density and potential are known, the velocity dispersion can be determined.
 Publication:

Monthly Notices of the Royal Astronomical Society
 Pub Date:
 February 1989
 DOI:
 10.1093/mnras/236.4.801
 Bibcode:
 1989MNRAS.236..801E
 Keywords:

 Hydrodynamic Equations;
 Stellar Motions;
 Boundary Value Problems;
 Green'S Functions;
 Stress Tensors;
 Velocity Distribution;
 Astrophysics