Statistics – Computation
Scientific paper
Oct 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992mnras.258..587e&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 258, no. 3, p. 587-598.
Statistics
Computation
2
Celestial Mechanics, Disks (Shapes), Kinematics, Spheroids, Stellar Physics, Stellar Structure, Astronomical Models, Computational Astrophysics, Cosmology, Density Distribution, Gravitational Collapse, Hydrodynamic Equations
Scientific paper
Solutions of the equations of stellar hydrodynamics for disks and spheroids are given. Unlike previous investigations, the velocity ellipsoid is aligned on confocal quadric surfaces rather than the simpler but less realistic spherical polar or cylindrical polar coordinate surfaces. The spheroidal models behave as if the velocity ellipsoids are aligned in cylindrical polars close to the center but in spherical polars asymptotically. For oblate spheroids, the velocity ellipsoids are largest at the position of the focus of the spheroidal coordinates, but diminish and become isotropic in the core. When viewed at inclinations of 40 percent or greater, radially anisotropic oblate spheroids show a peak in the line-of-sight velocity dispersion along the isophotal minor axis at or just beyond the projected position of the focus. For prolate spheroids, the velocity ellipsoids are usually largest at the center. It is concluded that the existence of a maximum in the velocity dispersion, offset from the center along the minor axis, is a signature of oblate models dominated by radial anisotropy in the outer parts and generated by distribution functions depending on three integrals of motion.
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