In the paper, the location of liberation points have been observed and triangular liberation points L4 and L5 are determined. DOI: http://dx.doi.org/10.3126/bibechana.v9i0.7185 BIBECHANA 9 (2013) 121-125

This paper deals with the transformation of KS-Variables and canonically conjugate variables from sideral (inertial) to synodic (rotating) form and their applications in "the circular restricted problem of three bodies in three-dimensional coordinate system" to form generating solutions.

The solutions of sitnikov's circular restricted three body problem has been tried to obtain by using Lindstedt poincare method if the primaries are oblate spheroid. DOI: http://dx.doi.org/10.3126/bibechana.v10i0.9340   BIBECHANA 10 (2014) 92-99

In this paper we have been examined the stability of the perturbed solutions of the restricted three body problem. We have been restricted ourselves only to the first order variational equations. Our variational equations depend on the periodic solutions. Here the applications of the method of Fuchs and Floquet Proves to be complicated and hence we have been preferred Poincare's Method of determination of the characteristic exponents. With the determination of the characteristic exponents we have been abled to conclude regarding the stability of the generating solution. We have obtained that the motions are unstable in all the cases. By Poincare's implicit function theorem we have concluded that the stability would remain the same for small value of the parameter  and in all types of motion of the restricted three-body problem.©RCOST: All rights reserved.

The Sitnikov's problem is a special case of restricted three body problem if the primaries are of equal masses (m 1 = m 2 = 1/2) moving in circular orbits under Newtonian force of attraction and the third body of mass m 3 moves along the line perpendicular to plane of motion of primaries. Here oblate spheroid primaries are taken. The solution of the Sitnikov's circular restricted three body problem has been checked when the primaries are oblate spheroid. We observed that solution is depended on oblate parameter A of the primaries and independent variable t. τ = η For this the stability of non-trivial solutions with the characteristic equation is studied. The general equation of motion of the infinitesimal mass under mutual gravitational field of two oblate primaries are seen at equilibrium points. Then the stability of infinitesimal third body m 3 has been calculated.