THE EFFECT OF TEMPERATURE EVOLUTION ON THE INTERIOR STRUCTURE OF H2O-RICH PLANETS

@article{Zeng2014THEEO,
  title={THE EFFECT OF TEMPERATURE EVOLUTION ON THE INTERIOR STRUCTURE OF H2O-RICH PLANETS},
  author={Li Zeng and Dimitar D. Sasselov},
  journal={The Astrophysical Journal},
  year={2014},
  volume={784},
  pages={96}
}
For most planets in the range of radii from 1 to 4 R ⊕, water is a major component of the interior composition. At high pressure H2O can be solid, but for larger planets, like Neptune, the temperature can be too high for this. Mass and age play a role in determining the transition between solid and fluid (and mixed) water-rich super-Earth. We use the latest high-pressure and ultra-high-pressure phase diagrams of H2O, and by comparing them with the interior adiabats of various planet models, the… 

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References

SHOWING 1-10 OF 20 REFERENCES
The phase diagram of water and the magnetic fields of Uranus and Neptune
Abstract The interior of giant planets can give valuable information on formation and evolution processes of planetary systems. However, the interior and evolution of Uranus and Neptune is still
A Detailed Model Grid for Solid Planets from 0.1 through 100 Earth Masses
This article describes a new grid for the mass-radius relation of three-layer exoplanets within the mass range of 0.1-100 M⊕. The three layers are: Fe (-phase of iron), MgSiO3 (including both the
The Interior Dynamics of Water Planets
The ever-expanding catalog of detected super-Earths calls for theoretical studies of their properties in the case of a substantial water layer. This work considers such water planets with a range of
The effect of composition on the evolution of giant and intermediate-mass planets
ABSTRACT We model the evolution of planets with various masses and compositions. We investigatethe effects of the composition and its depth dependence on the long-term evolution of theplanets. The
Water/Icy Super-Earths: Giant Impacts and Maximum Water Content
Water-rich super-Earth exoplanets are expected to be common. We explore the effect of late giant impacts on the final bulk abundance of water in such planets. We present the results from smoothed
Volatile Transport inside Super-Earths by Entrapment in the Water Ice Matrix
Whether volatiles can be entrapped in a background matrix composing planetary envelopes and be dragged via convection to the surface is a key question in understanding atmospheric fluxes, cycles and
Superionic and metallic states of water and ammonia at giant planet conditions.
TLDR
The phase diagrams of water and ammonia were determined by constant pressure ab initio molecular dynamic simulations at pressures (30 to 300 gigapascal) and temperatures (300 to 7000 kelvin) of relevance for the middle ice layers of the giant planets Neptune and Uranus to improve the understanding of the properties of the middle icy layers.
A super-Earth transiting a nearby low-mass star
TLDR
Observations of the transiting planet GJ’1214b are reported, finding that the planetary mass and radius are consistent with a composition of primarily water enshrouded by a hydrogen–helium envelope that is only 0.05% of the mass of the planet.
Numerical dynamo models of Uranus' and Neptune's magnetic fields
Abstract The non-axisymmetric, non-dipolar magnetic fields of Uranus and Neptune are markedly different from the axially-dipolar dominated fields of the other planets in our Solar System with active
High pressure ices
TLDR
H2O will be more resistant to metallization than previously thought, and a sequence of new stable and meta-stable structures for the ground state of ice in the 1–5 TPa (10 to 50 Mbar) regime is found, in the static approximation.
...
1
2
...