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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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The orbit of 2010 TK7. Possible regions of stability for other Earth Trojan asteroids
TL;DR: In this article, the authors derived an analytical mapping in the spatial elliptic restricted three-body problem to find the phase space structure of the dynamical problem and used precise numerical methods to integrate the orbit forward and backward in time in different dynamical models.
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Capture into first-order resonances and long-term stability of pairs of equal-mass planets
TL;DR: In this paper, the authors studied the stability of resonant systems as a function of planetary mass and showed that the resonant system is more stable than non-resonant ones for a given minimal distance at close encounters.
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Secular increase of the Astronomical Unit: a possible explanation in terms of the total angular momentum conservation law
TL;DR: In this paper, the authors give an idea and the order-of-magnitude estimations to explain the recently reported secular increase of the Astronomical Unit (AU) by Krasinsky and Brumberg (2004).
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Orbits, masses, and evolution of main belt triple (87) sylvia
TL;DR: Sylvia is a triple asteroid system located in the main belt as mentioned in this paper, which is composed of a dominant central mass surrounded by two satellites orbiting at 706.5 2.5 km and 1357 4.0 km.