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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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Resonance Overlap Is Responsible for Ejecting Planets in Binary Systems
Lawrence Mudryk,Yanqin Wu +1 more
TL;DR: In this article, it was shown that the Hill criterion yields an instability boundary that is very similar to that obtained by resonance overlap arguments, making the former both a necessary and a sufficient condition for planet instability.
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The population of natural Earth satellites
Journal ArticleDOI
Heliospheric Coordinate Systems
Markus Fränz,D. Harper +1 more
TL;DR: In this paper, the most common coordinate systems used in space science have been described in previous work and extended to systems used for physical observations of the Sun and the planets and to systems based on spacecraft location.
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Simulations of planet migration driven by planetesimal scattering
TL;DR: Ida et al. as discussed by the authors showed that a bias in scattering timescales on either side of the planet's orbit leads to a very strong tendency for the planet to migrate inwards, towards the star instead of outwards.
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A Dynamical Analysis of the Kepler-80 System of Five Transiting Planets
Mariah G. MacDonald,Darin Ragozzine,Darin Ragozzine,Darin Ragozzine,Daniel C. Fabrycky,Eric B. Ford,Matthew J. Holman,Howard Isaacson,Jack J. Lissauer,Eric D. Lopez,Tsevi Mazeh,Leslie A. Rogers,Jason F. Rowe,Jason F. Rowe,Jason H. Steffen,Guillermo Torres +15 more
TL;DR: In this paper, the outer four planets are in a rare dynamical configuration with four interconnected three-body resonances that are librating with few degree amplitudes, and they are assumed to have similar masses but different radii.