Hostname: page-component-77c89778f8-fv566 Total loading time: 0 Render date: 2024-07-18T16:09:43.660Z Has data issue: false hasContentIssue false
  • English
  • Français

Galactic Orbits of Different Galactic Population Objects

Published online by Cambridge University Press:  25 May 2016

L. P. Ossipkov  and
S. A. Kutuzov
L. P. Ossipkov
Affiliation:
St Petersburg State University, Stary Peterhof, St Petersburg 198904, Russia
S. A. Kutuzov
Affiliation:
St Petersburg State University, Stary Peterhof, St Petersburg 198904, Russia

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.

It is evident that the knowledge of not only positions and velocities of objects belonging to different populations but also their osculating galactic orbits can clarify the structure and history of our Galaxy. Action variables being adiabatic invariants are especially useful for these purposes (Binney, May 1986). One of them is a usual area integral (and it can be found without any orbit calculation). The second action variable is connected with an energy integral but for 3–D orbits and arbitrary potentials it cannot be found analitically. Eccentricities resulting from orbit calculations can be used here (Lynden-Bell 1963). Comparison of eccentricities defined with different ways shown that differences between them are practically negligible (Kutuzov 1985, 1987). As for the third action variable and the corresponding third isolating integral orbit calculations can confirm its existence and control the validity of various approximations. Numerical technique allowing to find it and working at any potential is now in progress (Binney, Kumar 1993).

Type
Chapter 6: How are we to Understand the Large Scale Structure of the ISM?
Information
Symposium - International Astronomical Union , Volume 169: Unsolved Problems of the Milky Way , 1996 , pp. 523 - 524
Copyright
Copyright © Kluwer 1996 

References

Allen, C., Santillan, A. (1993) Rev. Mex. Astron. Astrof. , Vol. 25, p.39.Google Scholar
Allen, C., Schuster, W., Poveda, A. (1991) AA , Vol. 244, p. 286.Google Scholar
Binney, J., May, A. (1986) MN , Vol. 218, p. 743.Google Scholar
Binney, J., Kumar, S. (1993) MN , Vol. 261, p. 584.Google Scholar
Cudworth, K.M. (1974) AJ , Vol. 80, p.199.Google Scholar
Cudworth, K.M., Hanson, R.M. (1993) AJ , Vol. 105, p. 168.CrossRefGoogle Scholar
Khromov, G.S. (1985) Planetary Nebulae , Nauka, Moscow.Google Scholar
Kutuzov, S.A. (1985) Astronomical and Geodetical Studies , ed. Barkhatova, K.A. Ural Univ. Press, Sverdlovsk, p.56.Google Scholar
Kutuzov, S.A. (1987) Kin. i fiz. neb. tel , Vol.3, No 4, p.11.Google Scholar
Kutuzov, S.A., Ossipkov, L.P. (1989) AZh , Vol. 66, p. 965.Google Scholar
Lynden–Bell, D. (1963) Observatory , No 932, p. 232.Google Scholar
Ossipkov, L.P. (1976) Pis'ma v AZh , Vol. 2, p. 367.Google Scholar
Ossipkov, L.P., Kutuzov, S.A. (1993) Galactic Bulges , ed. Dejonghe, H., Habing, H.J. Kluwer, Dordrecht, p.369.Google Scholar
Villumsen, J.V., Binney, J. (1985) ApJ , Vol. 295, p.388.Google Scholar