Solutions of the equations of stellar hydrodynamics for Eddington systems

Details Solutions of the equations of stellar hydrodynamics for Eddington systems Solutions of the equations of stellar hydrodynamics for Eddington systems

Feb 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989mnras.236..801e&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 236, Feb. 15, 1989, p. 801-816. Research supported by S

Astronomy and Astrophysics

Astronomy

17

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

Scientific paper

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.

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