Models of Uranus and Neptune

The problem of the models of Uranus and Neptune is examined in this survey. The results of detailed constructions of three-layer models are presented. The models of Uranus and Neptune are divided into two classes (models without neon and models with neon enrichment) corresponding to whether the mechanism for gas dissipation from the solar nebula was hydrodynamic or thermal. The best three-layer models without neon are the type T6 models (content of about 25 percent CH4 and NH3 in the outer hydrogen-helium mantle). Purely formally, best satisfying the observational data are the models with neon enrichment by 40 times, for which the ratio of the ice component to the heavy component IC/HC is about 2.6-2.65 by Mass. For these models J4_U = -4.36 x 10 to the 5th, J2_N = 3.84 x 10 to the -3rd J4_N = -2.82 x 10 to the -5th. The dynamic oblatenes of Uranus agrees well with that observed optically, while the dynamic oblatenes of Neptune is somewhat less than the average oblateness observed optically.