Monte Carlo interior models for Uranus and Neptune

Details Monte Carlo interior models for Uranus and Neptune Monte Carlo interior models for Uranus and Neptune

Nov 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995jgr...10023349m&link_type=abstract

Journal of Geophysical Research, Volume 100, Issue E11, p. 23349-23354

Physics

15

Planetology: Fluid Planets: Interiors, Planetology: Fluid Planets: Composition, Planetology: Solar System Objects: Uranus, Planetology: Solar System Objects: Neptune

Scientific paper

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, rotation rate, radius, and gravitational moments of the two planets. New models with a composition gradient in the outer third of the planetary radius are found for both planets. Such composition gradients may play a significant role in controlling the internal heat flow. In agreement with previous models, we find that the pressure-density relation for the central third of both planets is consistent with either ice or a mixture of materials with a similar equation of state. While the range of allowed models is now somewhat greater, the principal conclusions drawn from traditional interior modeling techniques are robust.

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