Abstract
It is well known that the triangular points of the restricted three-body problem are linearly stable for the mass ratio \(0\langle\mu\langle{\mu_0}=\frac{1}{2}-\sqrt{69}/18=0.03852089\ldots\), the critical mass value. The range of the mass parameter giving rise to stable triangular solutions decreases when the more massive primary (Subba Rao — Sharma, 1975) or both the primaries (Bhatnagar — Hallan, 1979) are oblate spheroids with their equatorial planes coincident with the plane of motion. If the more massive primary is a source of radiation, the value of critical mass decreases with the increase in the radiation force (Chernikov,1970).
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References
Bhatnagar, K.B. and Iiallan, P.P. (1979), Celes. Mech., 20, 95–103.
Chernikov, Y.A. (1970), Astron. Z., 47, 217–223.
Sharma, R.X. and Subba Rao, P.V. (1979) Astrophys. And Space Sci., 60, 247–250.
Subba Rao, P.V. and Sharma, R.I. (1975), Astron. Astrophys., 43, 381–383.
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© 1982 D. Reidel Publishing Company
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Sharma, R.K. (1982). On Linear Stability of Triangular Libration Points of the Photogravitational Restricted Three-Body Problem Wien the More Massive Primary is an Oblate Spheroid. In: Fricke, W., Teleki, G. (eds) Sun and Planetary System. Astrophysics and Space Science Library, vol 96. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-7846-1_114
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DOI: https://doi.org/10.1007/978-94-009-7846-1_114
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