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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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Motion of dust in mean motion resonances with planets
TL;DR: In this article, the authors investigated the effect of stellar electromagnetic radiation on the motion of a spherical particle in mean motion orbital resonances with a planet and showed that it is sufficient to allow either nonzero eccentricity of the planet or nonsphericity of the grain and the orbital evolutions in the resonances are qualitatively equal for the two cases.
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Effects of Turbulence, Eccentricity Damping, and Migration Rate on the Capture of Planets into Mean Motion Resonance
TL;DR: In this article, the authors studied the convergent migration of giant planets and determined the probability that they are captured into mean motion resonance, which depends on the type of resonance, the migration rate, the eccentricity damping rate, and the amplitude of the turbulent fluctuations.
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Gravitational effects of Nix and Hydra in the external region of the Pluto–Charon system
TL;DR: Weaver et al. as mentioned in this paper analyzed the dynamical structure of the external region of the Pluto-Charon binary system by numerically simulating a sample of particles under the gravitational effects of Pluto, Charon, Nix and Hydra.
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Relativistic Effects in Extrasolar Planetary Systems
Fred C. Adams,Gregory Laughlin +1 more
TL;DR: In this article, general relativistic (GR) effects in currently observed extrasolar planetary systems were considered, and it was shown that GR corrections can compete with secular interactions in these systems and thereby play an important role.
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Stellar dynamics around a massive black hole – I. Secular collisionless theory
S. Sridhar,Jihad R. Touma +1 more
TL;DR: The collisionless Boltzmann equation (CBE) for the stellar distribution function (DF) is averaged over the fast Kepler orbital phase using the method of multiple scales as mentioned in this paper.