Titlebook: Qualitative and Quantitative Behaviour of Planetary Systems; Proceedings of the T R. Dvorak,J. Henrard Conference proceedings 1993 Kluwer A

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Review of Planetary and Satellite Theoriesobservational data, and the requirements of the astronomical community. Thus, the development of computers made it possible to replace planetary and lunar general theories with numerical integrations, or special perturbation methods. In turn, the availability of inexpensive small computers and high-

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The Mystery of Pluto’s Massstence of a ring of billions of small satellites about Pluto up to tenths of millions of kilometers..The stability, the shape and the dimensions of such an heavy ring are discussed..Finally a general review of advantages and drawbacks of this ring theory is presented as well as the possibilities of

PAC

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Stable Planetary Orbits Around One Component in Nearby Binary Stars. IInd one of the two components in double stars can exist. For any given set of initial parameters (the mass ratio of the two stars and the eccentricity of their orbit around each other), the phase-space of initial positions and velocities is systematically explored..In previous works, systematic explo

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UNT

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Numerical Results to the Sitnikov-Problemhe two primaries have equal masses and the third body moves perpendicular to the plane of the primaries’ orbit through their barycenter. The circular problem is integrable through elliptic integrals; the elliptic case offers a surprisingly great variety of motions which are until now not very well k

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A Computer Aided Analysis of the Sitnikov Problemn ellipses. The zero mass body intersects the primaries plane at the systems barycenter. This problem is commonly known as the .. In this work we are looking for a first integral related to the oscillatory motion of the zero mass body. This is done by first expressing the equation of motion by a sec

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The Original Sitnikov Article — New Insightsarch 1960 is reexamined, because of several shortcomings found in the paper. For the first time Sitnikov presented the following nontrivial result: There exists a class of orbits in the three body problem which are unbounded, but nevertheless lead back to the origin of the coordinate system used, an

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