Liquid Water Oceans in Ice Giants

@article{Wiktorowicz2007LiquidWO,
  title={Liquid Water Oceans in Ice Giants},
  author={Sloane J. Wiktorowicz and Andrew P. Ingersoll},
  journal={Icarus},
  year={2007},
  volume={186},
  pages={436-447}
}

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References

SHOWING 1-10 OF 45 REFERENCES
The interior of Neptune
Neptune, together with Uranus, belongs to the ice-rich class of Jovian planets. Although molecular hydrogen is the dominant species in its atmosphere, all available evidence points toward an
The Origin of Carbon Monoxide in Neptune's Atmosphere
The CO abundance in the observable atmosphere of Neptune can be plausibly explained by rapid vertical mixing from the deeper atmosphere if Neptune has a greater complement of water than Uranus.
Models of Uranus' interior and magnetic field
Our understanding of Uranus' interior structure comes from the results of theoretical models. In this chapter, we review the methods for computing such models. We discuss the various physical
Monte Carlo interior models for Uranus and Neptune
To explore a greater realm of model phase space than has previously been mapped, we generate randomly chosen interior models for Uranus and Neptune. The models are constrained by the observed mass,
Convective-region geometry as the cause of Uranus' and Neptune's unusual magnetic fields
TLDR
Three-dimensional numerical dynamo simulations that model the dynamo source region as a convecting thin shell surrounding a stably stratified fluid interior produce magnetic fields similar in morphology to those of Uranus and Neptune.
The Abundances of Methane and Ortho/Para Hydrogen on Uranus and Neptune: Implications of New Laboratory 4-0 H2 Quadrupole Line Parameters
Abstract The tropospheric methane molar fraction (ƒ CH 4. t ) and the ortho/para hydrogen ratio are derived for Uranus and Neptune based on new determinations of spectroscopic parameters for key
Further investigations of random models of Uranus and Neptune
An extrasolar planetary system with three Neptune-mass planets
TLDR
Simulations show that the system of three Neptune-mass planets orbiting the nearby star HD 69830 is in a dynamically stable configuration and theoretical calculations favour a mainly rocky composition for both inner planets, while the outer planet probably has a significant gaseous envelope surrounding its rocky/icy core.
Neptune and Triton
The first reconnaissance of all the major planets of the Solar System culminated in the Voyager 2 encounter with Neptune in August 1989. Neptune itself was revealed as a planet with gigantic active
Interiors of the Giant Planets
TLDR
The distribution and relative amounts of these components in the interiors of the Jovian planets can be inferred from theoretical and expermental data on equations of state and from the planets' hydrostatic equilibrium response to rotation.
...
...