Nonadiabatic models of Jupiter and Saturn

Details Nonadiabatic models of Jupiter and Saturn Nonadiabatic models of Jupiter and Saturn

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994icar..112..354g&link_type=abstract

Icarus (ISSN 0019-1035), vol. 112, no. 2, p. 354-367

Astronomy and Astrophysics

Astronomy

52

Abundance, Astronomical Models, Jupiter (Planet), Nonadiabatic Conditions, Saturn (Planet), Temperature Profiles, Convective Flow, Equations Of State, Helium, Phase Transformations, Thermodynamics

Scientific paper

New interior models for Jupiter and Saturn are described that do not assume the temperature profiles to be adiabatic throughtout the entire hydrogen-helium envelope. These models include the recently calculated radiative opacities due to hydrogen, helium, water, methane, and ammonia and an up-to-date hydrogen/helium equation of state. The helium abundnace in the planet, the mass of the core, and the discontinuity of helium abundance at the molecular/metallic hydrogen phase transition (or the ice fraction in the core) are optimized to reproduce the observed mass, radius, and gravitational moments within their error bars. These nonadiabatic models are characterized by the presence of a radiative zone in the outermost layers of the planet, surrounded by two convective zones. This radiative window yields a substantial modification of the thermal properties of the planets and leads to cooler interior models. The mass of Jupiter core is found to be slightly larger than for the adiabatic models. Finally, the mass fractions of heavy elements deduced from our calculations are in better agreement with the values inferred from atmospheric measurements.

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