Hostname: page-component-7b7567c8c-2n9c9 Total loading time: 0 Render date: 2026-11-15T12:48:52.287Z Has data issue: false hasContentIssue false
  • English
  • Français

Orbital elements of different Galactic population objects

Published online by Cambridge University Press:  07 August 2017

L.P. Ossipkov and
S.A. Kutuzov
L.P. Ossipkov
Affiliation:
St. Petersburg University, Russia
S.A. Kutuzov
Affiliation:
St. Petersburg University, 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.

The study of prevalent orbits in galactic subsystems can help us understand galactic structure and clarify its history. The classical analysis of flat orbits and metallicities of old stars led Eggen et al. (1962) to formulate the rapid collapse of the primordial Galaxy. On the other side Yoshii & Saio (1979) studied three-dimensional orbits that separate in spherical coordinates. They found the Galaxy contracted quasi-stationary after the formation of halo objects. Here we shall briefly discuss the results of numerical orbit calculations (with Merson's method) for selected galactic subsystems. The axially symmetrical two-component model of the Galaxy (Kutuzov, Ossipkov 1989) was adopted. One-component models (Barkhatova et al. 1987, Kutuzov 1988) were used also but no significant difference in orbit elements was found (Kutuzov & Ossipkov 1992). Pericenter and apocenter distances, Rp and Ra , and the maximal height of objects over the galactic plane, zm , were used as orbit elements as well as dimensionless quantities e = (Ra — Rp )/(Ra + Rp ) (eccentricity) and c = 2zm /(Ra — Rp ) (the flatness of box filled by orbit projection on the meridional plane).

Information

Type
Contributed Papers
Information
Symposium - International Astronomical Union , Volume 153: Galactic Bulges , 1993, pp. 369 - 370
Copyright
Copyright © Kluwer 1993 

References

Barkhatova, K.A., Kutuzov, S.A., Ossipkov, L.P., 1987, Astr. Zh., 64, 956 Google Scholar
Clube, S.V.M., Aslan, Z., Russo, T.W., Clements, E.D., 1971, ROB, nd, 166, 175 Google Scholar
Cudworth, K.M. 1974, A.J., 79, 1384 CrossRefGoogle Scholar
Eggen, O.J., Lynden-Bell, D., Sandage, A.R., 1962, A.J., 136, 748 CrossRefGoogle Scholar
Hayli, A., 1965, An.d'Ap., 28, 49 Google Scholar
Hemenway, M.K., 1975, A.J., 80, 199 CrossRefGoogle Scholar
Innanen, K.A., 1966, Z. f. Ap., 80, 445 Google Scholar
Khromov, G.S., 1985, Planetarnye tumannosti. Nauka, Moscow Google Scholar
Kutuzov, S.A., 1988, Kin. fiz. neb. tel, 4, 39 Google Scholar
Kutuzov, S.A., Ossipkov, L.P., 1989, Astrono. Zh., 66, 965 Google Scholar
Kutuzov, S.A., Ossipkov, L.P., 1992, In: Astron.-geodez. issl., Ural Univ. Press, Ekaterinburg (in press) Google Scholar
Perek, I., Kohoutek, L. 1967, Catalogue of galactic planetary nebulae, Academia, Prague Google Scholar
Woolley, R., Harding, G.A., Cassels, I. 1965, ROB, nd, 97, E3 Google Scholar
Yoshii, Y., Saio, H. 1979, PASP, 31, 339 Google Scholar