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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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Tidal Friction and Tidal Lagging. Applicability Limitations of a Popular Formula for the Tidal Torque
TL;DR: In this paper, the authors explain why the derivation of this expression, offered in the paper by Goldreich (1966; AJ 71, 1 - 7) and in the books by Kaula (1968, eqn. 4.5.29), and Murray & Dermott (1999, 4.159), implicitly sets the time lag to be frequency independent, i.e., the same for all Fourier modes in the spectrum of tide.
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Asteroid families in the first-order resonances with Jupiter
Miroslav Brož,David Vokrouhlický +1 more
TL;DR: In this paper, the Yarkovsky effect (infrared thermal emission from the surface of asteroids) causes a systematic drift in eccentricity for resonant asteroids, while their semimajor axis is almost fixed due to the strong coupling with Jupiter.
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Secular Interactions between Inclined Planets and a Gaseous Disk
TL;DR: In this article, the authors investigated the normal modes of mutually inclined planet-disk systems and determined the normal mode of some mutually inclined system-disk system systems with a gaseous protostellar disk that may contain a nodal particle resonance.
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A criterion to classify asteroids and comets based on the orbital parameters
TL;DR: In this article, the authors proposed a criterion to classify asteroids and comets and to find the border case based on the Tisserand's parameter, the Minimum Orbital Intersection Distance (MOID), and considering some information regarding the aphelion and perihelion distances.
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Karin cluster formation by asteroid impact
TL;DR: In this article, the authors studied the Karin cluster, a small asteroid family that formed 5.8 ± 0.2 Myr ago in the outer main belt and found that the parent body material was ejected as fragments ranging in size from sub-km to dust grains.