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The Libration Points and Hill Surfaces in the Restricted Problem of Three Variable-Mass Bodies

Published online by Cambridge University Press:  12 April 2016

A.A. Bekov
A.A. Bekov*
Affiliation:
Institute of Astrophysics, Kazakh SSR, Academy of Sciences, 480068 Alma-Ata, Russia

Abstract

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The paper deals with the study of the arising and disappearence of collinear (Eulerian) L1, L2, L3, triangular (Lagrangian) L4, L5, coplanar L6, L7, ring L0 and infinitely distant L±∞ solutions in a restricted problem of three variable-mass bodies for different time dependencies of main bodies masses and for some additional conditions imposed on the systems parameters. In this case it is assumed that the motion of variable-mass main bodies is determined by the Gylden-Mestschersky problem. The Bill surfaces in the restricted three-body problem where main bodies masses variate isotropically according to the Mestschersky law are studied. Certain possibilities of applying the results of investigations to nonstationary double stellar systems are discussed.

Type
Part IV Triple and Many Body Problem
Information
International Astronomical Union Colloquium , Volume 132: Instability, Chaos and Predictability in Celestial Mechanics and Stellar Dynamics , 1993 , pp. 277 - 288
Copyright
Copyright © Nova Science Publishers 1993

References

[1] Bekov, A.A. (1987). The Latours of Astrophys. Inst, of Academy of Sciences of Kazakh SSR, Alma-Ata. 47, 12.Google Scholar
[2] Bekov, A.A. (1988), Astron. J. of Academy of Sciences of USSR, 65, 202.Google Scholar
[3] Bekov, A.A. (in preparation).Google Scholar
[4] Bekov, A.A. (in press).Google Scholar
[5] Gelfgat, B.E. (1973), Current problems of celest.Mech. and Astrodynamics, Moscow, p.7.Google Scholar
[6] Gylden, H. (1884), Astron. Nachr. 109, 1.CrossRefGoogle Scholar
[7] Horedt, G.P. (1984), Celest. Mech. 33, 367.CrossRefGoogle Scholar
[8] Luk’yanov, L.G. (1988), Astron. J. of Academy of Sciences of USSR, 65, 1308.Google Scholar
[9] Luk’yanov, L.G. (1989a), Astron. J. of Academy of Sciences of USSR, 66, 180.Google Scholar
[10] Luk’yanov, L.G. (1989b), Astron. J. of Academy of Sciences of USSR, 66, 385.Google Scholar
[11] Mestschersky, I.W. (1902), Astron. Nachr. 159, 229.CrossRefGoogle Scholar
[12] Orlov, A.A. (1939), Astron. J. of Academy of Sciences of USSR, 16, 52.Google Scholar
[13] Sersic, J.L. (1970), Periodic orbits, stability and resonces (edited by Giacaglia, G.E.O.), Dordrecht, p.314. CrossRefGoogle Scholar
[14] Sersic, J.L. (1973), Bill. Astron. Inst. Czechoslovakia, 24, 150.Google Scholar
[15] Singh, J., Ishwar, B., (1984), Celest. Mech. 32, 297.CrossRefGoogle Scholar