Giant planets convection

Boss, A. P. (2004) Convective cooling of protoplanetary disks and rapid giant planet formation. Astrophysical Journal, 610, 456-463. 

As we have seen water is an important constituent of the giant planets besides hydrogen and helium. This was pointed out by Stevenson and Fishbein, 1981 [326]. The presence of water and other heavy molecules in the interiors of the giant planets may inhibit convection as a means of energy transport there. Guillot, 1995 [150] found that convection is inhibited in Uranus and Neptune when methane reaches an abundance of about 15 times the solar value and in Jupiter and Saturn if the abundance of water is more than about five times the solar value. Roos-Serote et al 2004 [280] studied the water abundance in the atmosphere of Jupiter by analysing the O/H ratio. This ratio was found compatible with one or more times the solar value. Water vapor is the main source for O (except some small contribution from CO). 

Guillot, T. Condensation of methane ammonia and water in the inhibition of convection in giant planets. Science 269,1697 (1995)... 

Hueso, R., Sanchez-Lavega, A. A three-dimensional model of moist convection for the giant planets II Saturn s water and ammonia moist convective storms. Icarus 172,255-271 (2004) Hui, L., Seager, S. Atmospheric lensing and oblateness effects during an extrasolar planetary transit. Astrophys. J. 572, 540-555 (2002)... 

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