Are the Giant Planets Fully Convective?

✍ Scribed by T. Guillot; D. Gautier; G. Chabrier; B. Mosser

• Publisher: Elsevier Science
• Year: 1994
• Tongue: English
• Weight: 949 KB
• Volume: 112
• Category: Article
• ISSN: 0019-1035
• DOI: 10.1006/icar.1994.1188

✦ Synopsis

All current models of internal structure and evolution of the giant planets assume a convective and adiabatic stratification. The purpose of this work is to reexamine this hypothesis using the most recent available opacity data. Rosseland opacities are calculated for density and temperature conditions relevant to the fluid molecular envelope of the giant planets and for the compositions inferred from atmospheric measurements. These opacities include the absorption by hydrogen, helium, water, methane, and ammonia. The contribution of metals to the electron abundance is also taken into account. The region investigated covers temperatures from 200 to (5000 \mathrm{~K}) and densities from (10^{-4}) to (0.5 \mathrm{~g} \mathrm{~cm}^{-3}).

It is shown that giant planets of pure hydrogen and helium may not be fully convective for temperatures below (\sim 4000 \mathrm{~K}). The opacity due to water and methane is very strong at low temperature levels but is insufficient to restore convection around (\sim 2000 \mathrm{~K}) in Jupiter and Saturn; however, the lack of data precludes us from safely modeling the ammonia opacity at wavenumbers higher than (2000 \mathrm{~cm}^{-1}). Our calculations also predict a radiative zone in Uranus but the uncertainty in the value of the opacity prevents any firm conclusion. The fluid envelope of Neptune seems to be entirely convective. The possible influence on the absorption of heavy constituents other than (\mathrm{CH}{4}, \mathrm{NH}{3}), and (\mathrm{H}_{2} \mathrm{O}) is discussed. 1994 Academic Press, Inc.