Constraints on the origin and interior structure of the major planets

Details Constraints on the origin and interior structure of the major planets Constraints on the origin and interior structure of the major planets

Dec 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981rspta.303..315h&link_type=abstract

(Royal Society, Discussion on Planetary Exploration, London, England, Nov. 4, 5, 1980.) Royal Society (London), Philosophical Tr

Computer Science

5

Atmospheric Composition, Atmospheric Models, Gas Giant Planets, Planetary Atmospheres, Planetary Evolution, Planetary Structure, Abundance, Atmospheric Tides, Constraints, Gravitational Fields, Heat Transfer, Space Exploration, Planets, Origin, Interiors, Structure, Models, Giant Planets, Uranus, Neptune, Jupiter, Saturn, Comparisons, Cores, Composition, Enrichment, Deuterium, Abundance, Heat Flow, Gravity Fields, Parameters, Diagrams, Atmosphere, Tidal Effects, Evolution, Layers, Thermal History

Scientific paper

Fitting models to the external gravity field of the major planets (Uranus, Neptune, Jupiter, and Saturn), it is found that certain interior characteristics may be common to all four. For Uranus and Neptune, a model with a central iron-silicate core of approximately four earth masses, an 'ice' layer of H2O, CH4, and NH3 in solar proportions of about 10 earth masses, and an H2-He atmosphere of about 1-2 earth masses gives a good fit to available constraints, including heat flow measurements. Models of Jupiter and Saturn have cores very similar to those of Uranus and Neptune; the H2-He layer, however, is markedly more extensive. Modes of origin that are consistent with these features are discussed. Models of this type predict a considerable enrichment of deuterium relative to primordial solar abundances in Uranus and Neptune. Such enrichment is not observed in Uranus; implications are discussed for interior structure and origin.

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