Hostname: page-component-cd9895bd7-gbm5v Total loading time: 0 Render date: 2024-12-12T09:42:01.228Z Has data issue: false hasContentIssue false
  • English
  • Français

Scale-Free Models of Elliptical Galaxies

Published online by Cambridge University Press:  04 August 2017

Douglas O. Richstone
Douglas O. Richstone*
Affiliation:
Department of Astronomy, University of Michigan

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

In this note I will report the general character of all scale-free solutions of the collisionless Boltzmann and Poisson equations for a specific shape. In this case, the density falls as r−2 along any radial ray, the potential is logarithmic with oblate spheroidal level surfaces, and the flattening corresponds to an E5 or E6 density distribution (see Richstone 1980, hereafter Paper I). Schwarzschild's (1979) method was used. Toomre (1982) has recently discussed the properties of scale free models of this sort with distribution functions dependent on only the two classical isolating integrals. The method used here automatically incorporates the third integral.

Type
V. Spheroidal Systems
Information
Symposium - International Astronomical Union , Volume 100: Internal Kinematics and Dynamics of Galaxies , 1983 , pp. 289 - 290
Copyright
Copyright © Reidel 1983 

References

Binney, J. J.: 1981, in The Structure and Evolution of Normal Galaxies (ed. by Fall, and Lynden-Bell, ) Cambridge University Press, pp. 55.Google Scholar
Richstone, D. O.: 1980, Astrophys. J. 238, pp. 103.CrossRefGoogle Scholar
Richstone, D. O.: 1982, Astrophys. J. 252, pp. 496.Google Scholar
Schwarzschild, M.: 1979, Astrophys. J. 232, pp. 236.Google Scholar
Toomre, A.: 1982, Astrophys. J. 259, pp. 535.Google Scholar