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Stability of Elliptical Galaxies. Theoretical Aspects

Published online by Cambridge University Press:  04 August 2017

V.L. Polyachenko
V.L. Polyachenko*
Affiliation:
Astrosovet, Ul. Pyatnitskaya 48, 109017 Moscow Sh–17, U.S.S.R.

Extract

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Stars, which contain more than 90% of the visible matter of the Universe, are organized into systems comprising a hierarchy of different masses and scales: from galactic stellar clusters to clusters of galaxies themselves. Most of the systems in this hierarchic sequence are collisionless: the characteristic time between collisions is much more than typical dynamical times (e.g., the period of oscillations). Various conditions of formation of collisionless gravitating systems leave traces on their main characteristic parameters—such as the angular momentum, the degree of anisotropy, the kind of dependence of the stellar density on coordinates, and so on. The lifetime of a system with a certain set of parameters depends essentially on whether these parameters belong to a region in which the system is stable, or not. If they do, the system may then exist practically without changes for an arbitrarily long time (in terms of the dynamical time scale); if they do not, it must quickly adjust to another, stable state.

Type
Invited Reviews
Information
Symposium - International Astronomical Union , Volume 127: Structure and Dynamics of Elliptical Galaxies , 1987 , pp. 301 - 314
Copyright
Copyright © Reidel 1987 

References

REFERENCES

Antonov, V.A., 1960. Astr. Zh., 37, 918 [1961. Soviet Astronomy, 4, 859].Google Scholar
Antonov, V.A., 1962. Vestn. Leningrad Univ., 19, 96.Google Scholar
Antonov, V.A., 1973. in Dynamics of Galaxies and Star Clusters, p. 139, ed.Google Scholar
Omarov, T.B., Nauka (Alma-Ata) (in Russian).Google Scholar
Barnes, J., Goodman, J., & Hut, P., 1986. Astrophys. J., 300, 112.CrossRefGoogle Scholar
Duncan, M.J., & Wheeler, J.C., 1980. Astrophys. J., 237, L27.CrossRefGoogle Scholar
Fridman, A.M., & Polyachenko, V.L. 1984. Physics of Gravitating Systems, Vols. 1 and 2, Springer Verlag (FP).Google Scholar
Fridman, A.M., & Shukhman, I.G., 1972. Dokl. Akad. Nauk SSSR, 202, 67 [Sov. Phys. Dokl., 17, 44].Google Scholar
Kuzmin, G.G., & Veitmann, Yu. I.K. 1968. Publ. Tartu Astroph. Obs., 36, 470.Google Scholar
Lynden–Bell, D., 1962. Mon. Not. R. astr. Soc., 124, 279.CrossRefGoogle Scholar
Lynden–Bell, D., & Sanitt, N., 1969. Mon. Not. R. astr. Soc., 143, 167.CrossRefGoogle Scholar
Marochnik, L.S., & Suchkov, A.A., 1974. Usp. Fiz. Nauk, 112, 275 [Sov. Phys. Usp., 17, 85].CrossRefGoogle Scholar
Merritt, D.R., & Aguilar, L.A., 1985. Mon. Not. R. astr. Soc., 217, 787.CrossRefGoogle Scholar
Michailovskii, A.B., Fridman, A.M., & Epel'baum, Ya.G. 1970. Zh. Eksp. Teor. Fiz., 59, 1608 [1971. Sov. Phys. JETP 32, 878].Google Scholar
Polyachenko, V.L., 1972. Kandidatskaja dissertatsija, Leningrad.Google Scholar
Polyachenko, V.L., 1981. Pis'ma Astr. Zh., 7, 142 [Soviet Astr. Lett., 7, 79].Google Scholar
Polyachenko, V.L., 1985. Astron. Tsirkular, 1405, 1.Google Scholar
Polyachenko, V.L., & Shukhman, I.G., 1972. Inst. Zemn. Magn. Ionosf. Rasprostr. Radiovoln Sibir. Otd. Akad. Nauk SSSR, 2–72, Irkutsk.Google Scholar
Polyachenko, V.L., & Shukhman, I.G., 1981. Astr. Zh., 58, 933 [Soviet Astronomy, 25, 533].Google Scholar
Shukhman, I.G., 1973. Astr. Zh., 50, 651 [Soviet Astronomy, 17, 415].Google Scholar
Synakh, V.S., Fridman, A.M., & Shukhman, I.G., 1971. Dokl. Akad. Nauk SSSR, 201(4), 827 [1972. Sov. Phys. Dokl., 16(12), 1062].Google Scholar
Vilenkin, N. Ya. 1968. Special Functions and Group Theory, Nauka, Moscow (in Russian).CrossRefGoogle Scholar