[地球流体電脳倶楽部] [dcmodel | dcmodel-tools] [dcmodel-thum.rb]

The equilibrium profiles of the Uranian atmospheres

Intro

The equilibrium profiles of the Uranian atmospheres are calculated to pass through the following temperature and pressure points that are determined from observations: 101 K at 2.3 times 10^{5} Pa from Lindal et al. [1987] for Uranus. All of the components considered in our calculations are listed as follows.

• Gas: H2, He, H2O, NH3, H2S, CH4
• Liquid: H2O, NH3, H2S, CH4
• Solid: H2O, NH3, H2S, CH4, NH4CH

H2O(l), NH3(l), and H2S(l) are assumed to form an ideal solution, while CH4(l) is isolated. Any combination of H2O(s), NH3(s), H2S(s), CH4(s), and NH4SH(s) is assumed not to be a solid solution. The ratio of ortho- to para-hydrogen is assumed to be that of the equilibrium value.

The abundances of non-condensible elements such as H and He are taken at the solar abundance, and the abundances of condensible elements, such as C, N, O, and S, are varied from 1 $ imes$ solar to 50 times solar abundance. The solar abundance adopted in the present study is that revised by Asplund et al. [2005], whereas that of Anders and Grevesse [1989] is used in the previous studies cited above. Each elemental abundance of He, C, N, O, and S is reduced from that of Anders and Grevesse [1989] by 13%, 33%, 46%, 46%, and 15%, respectively.

Output

obratmos_uranus_x10_434.0K-2.5d7Pa_stab.png	obratmos_uranus_x10_434.0K-2.5d7Pa_temp.png	obratmos_uranus_x1_451.0K-2.5d7Pa_stab.png
obratmos_uranus_x1_451.0K-2.5d7Pa_temp.png	obratmos_uranus_x30_596.0K-1.0d8Pa_stab.png	obratmos_uranus_x30_596.0K-1.0d8Pa_temp.png