Regular ArticleOrbital Stability of the Uranian Satellite System☆
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Cited by (57)
Keck near-infrared detections of Mab and Perdita
2023, IcarusOrbital stability of compact three-planet systems, I: Dependence of system lifetimes on initial orbital separations and longitudes
2021, IcarusCitation Excerpt :The first (lowest β value) upward spike found for five-planet systems by OVT17 started at ~ 8.6, but at that separation the trend in system lifetime is already higher, and the orbital spacing is closer to β values where most systems become very long-lived. That spike in lifetimes of 5-planet systems appears to be more closely analogous to the upturns in lifetimes at orbital separations that are “large” when expressed in mutual Hill radii that were found by Duncan and Lissauer (1997) and Duncan and Lissauer (1998), who varied the ratio of the masses of the (four or more) secondaries relative to that of the primary rather than the separation between orbits. Obertas et al. (2017) did not find any (five-planet) systems whose lifetimes are much more than one order of magnitude above their exponential fit until β > 8.3, and by that separation, the typical time to orbit crossing is already several million years.
The stability of tightly-packed, evenly-spaced systems of Earth-mass planets orbiting a Sun-like star
2017, IcarusCitation Excerpt :Numerical investigations of the stability of multi-planet (N ≥ 3) systems of planets in close orbits have been done (e.g., Chambers et al., 1996; Marzari and Weidenschilling, 2002; Smith and Lissauer, 2009; Pu and Wu, 2015; Tamayo et al., 2015; Morrison and Kratter, 2016), motivated by the consequences for planetesimal disks, closely-spaced multi-planet systems, and planet-induced gaps in debris disks. The same dynamics are relevant for Uranus’s inner satellites, with stability timescales orders of magnitude shorter than the age of the Solar System (Duncan and Lissauer, 1997; French and Showalter, 2012). Destined for close encounters, they have perhaps collided and re-formed throughout the history of the Solar System (French and Showalter, 2012).
Mab's orbital motion explained
2015, IcarusMUSE - Mission to the Uranian system: Unveiling the evolution and formation of ice giants
2015, Advances in Space ResearchThe science case for an orbital mission to Uranus: Exploring the origins and evolution of ice giant planets
2014, Planetary and Space ScienceCitation Excerpt :The inner moons of Uranus comprise the most densely-packed known satellite system, as can be seen in Fig. 7, with 13 known-objects on orbits ranging from 49,770 to 97,700 km (Cordelia to Mab) from the planet׳s centre. This crowded system appears to be subject to mutual collisions on timescales as short as ~106 yr (Duncan and Lissauer, 1997; Showalter and Lissauer, 2006; French and Showalter, 2012), and several moons show measurable orbital changes within a decade or less, raising important questions regarding the origin, evolution, and long-term stability of the Uranus system. Lying immediately exterior to Uranus׳ main ring system, but outside the “Roche limit” so that collisional products are able to re-accrete into new moons, these uranian inner satellites both interact with the rings (as well as with each other) and comprise a parallel system, a natural laboratory in which the effects of collisional disruption and re-accretion can be studied.
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J. T. BergstralhE. D. MinerM. S. Matthews, Eds.