Models of giant planets with a variable ratio of ice to rock

Details Models of giant planets with a variable ratio of ice to rock Models of giant planets with a variable ratio of ice to rock

May 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991angeo...9..357z&link_type=abstract

Annales Geophysicae (ISSN 0939-4176), vol. 9, May 1991, p. 357-366.

Astronomy and Astrophysics

Astronomy

19

Abundance, Astronomical Models, Gas Giant Planets, Planetary Evolution, Planetary Structure, Chemical Composition, Helium, Jupiter (Planet), Neptune (Planet), Saturn (Planet), Uranus (Planet)

Scientific paper

Numerical techniques are used to construct new models of the internal structure of Jupiter, Saturn, Uranus, and Neptune. New, significantly increased estimates of the abundance of helium give a new insight into the internal structures of Jupiter and Saturn and their cores. It is confirmed that the mass of Jupiter's core is several times smaller than Saturn's. Jupiter-like models of Uranus and Neptune with two-layer molecular envelopes are constructed. Models of the giant planets do not support Mizuno's hypothesis of approximately equal masses of embryos of the planets, on which the accretion of gas takes place. The assumption about the great depletion of carbon in Jupiter is discussed.

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