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1 atio in the atmospheres of Saturn, Titan and Uranus.
2 ellar ices in the cold nebular region beyond Uranus.
4 Extreme conditions inside ice giants such as Uranus and Neptune can result in peculiar chemistry and
6 er spacecraft discovered that the ice giants Uranus and Neptune have nondipolar magnetic fields, defy
7 The unusual magnetic fields of the planets Uranus and Neptune represent important observables for c
8 findings suggest that geophysical models of Uranus and Neptune require reassessment because chemical
9 uct ensembles of models for the interiors of Uranus and Neptune with the Concentric MacLaurin Spheroi
11 re-temperature condition in the interiors of Uranus and Neptune, forming a H(2)O-dominated fluid in t
23 e giants manifested by the low luminosity of Uranus, and lead to a better understanding of (exo-)plan
25 motion resonance among Jupiter, Saturn, and Uranus, and provides rough estimates of the Lyapunov tim
26 l importance for devising models of Neptune, Uranus, and white dwarf stars, as well as of extrasolar
29 the satellite systems of Jupiter, Saturn and Uranus arise naturally, and suggest that similar process
31 ow of the internal icy layers in Neptune and Uranus may be significantly faster than previously fores
32 ition of the interior of Neptune compared to Uranus means that the former is much more likely to cont
35 e to those present inside icy giant planets (Uranus, Neptune), shock-compressed polyethylene retains
37 n the interior of ice giant planets, such as Uranus or Neptune, are evaluated from equilibrium ab ini
44 cal properties of the ice giants Neptune and Uranus, there has been a growing interest in superionic