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Abstract: This paper presents the results of investigation of the orbital evolution of an extra-solar planet in a binary stellar system for one particular case, when the motion of its perigee is retarding and the orbit evolves to a circular orbit. Such planetary motion is characterized by a sufficiently large mutual inclination between the orbits of the distant star and the planet.
The planetary motion was considered in the frame of the general three-body problem, i.e. a planet in the close binary system revolving around one of the components. The distance between the stars is much greater than the semi-major axis of the planet's orbit. In differential equations of motion we used the Hamiltonian without short-periodic terms. As the intermediate orbit we used a non-Keplerian ellipse with the moving node and argument of perigee.
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Last update: May 30, 2006