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Solar system dynamics
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In this paper, the two-body problem and the restricted three body problem are considered. And the disturbing function is extended to include the spin-orbit coupling and the resonance perturbations.Abstract:
Preface 1 Structure of the solar system 2 The two-body problem 3 The restricted three-body problem 4 Tides, rotation and shape 5 Spin-orbit coupling 6 The disturbing function 7 Secular perturbations 8 Resonant perturbations 9 Chaos and long-term evolution 10 Planetary rings Appendix A Solar system data Appendix B Expansion of the disturbing function Indexread more
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Near-earth asteroid satellite spins under spin-orbit coupling
TL;DR: In this paper, the authors developed a fourth-order numerical integrator to simulate the coupled spin and orbital motions of two rigid bodies having arbitrary mass distributions under the influence of their mutual gravitational potential.
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Constraints on the original ejection velocity fields of asteroid families
TL;DR: In this paper, the inclination distribution of asteroids has been analyzed to understand the distribution of the component of the ejection velocity that is perpendicular to the orbital plane, and it was shown that the distribution should be more peaked than a Gaussian distribution, even if the initial distribution was Gaussian.
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Kozai resonance in extrasolar systems
TL;DR: In this paper, the authors considered the possibility that two-planar systems can be in a stable Kozai-resonant state, assuming a mutual inclination of the orbital planes of order.
Powering Triton's Recent Geological Activity by Obliquity Tides: Implications for Pluto Geology
Francis Nimmo,John R. Spencer +1 more
TL;DR: In this paper, the authors investigated the origins of Triton's deformed and young surface and found that the deformation is driven by obliquity tides, which arise because of its inclination.
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Secular dynamics of a coplanar, non‐resonant planetary system under the general relativity and quadrupole moment perturbations
TL;DR: In this article, a model of a coplanar system of N planets not involved in strong mean motion resonances, and which are far from collision zones, was constructed. But the model was not considered in this paper.