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Tidal interactions between Planet and its satellites are known to be the mainphenomena, which are determining the orbital evolution of the satellites. Wesuggest in the current research to take into consideration the additionalwell-known effect of differential rotation which obviously takes place in thegaseous or fluid convection zone of primary giant Planet (indeed, theaforementioned effect exists even not depending on the orbital evolution ofsatellites around host Planet). Nevertheless, estimations for the contributionof the aforementioned effect of differential rotation in the Uranus system(including all its most massive satellites) let us exclude using such effectfrom calculations of mutual evolution of the eccentricity e along with thesemi-major axis a for all satellites of Uranus (Planet of ice-type). It meansthat the Uranus can be considered in the analytic exploration of governingequations as to be the appropriate candidate for applying the modern ansatz[Efroimsky, 2015] (tidal dissipation effect depending on the tidal-flexurefrequency) in regard to estimations of eccentricity e along with semi-majoraxis a for satellites of Uranus. We can see from the results of calculations inSection 3 that the combined system of governing equations (in the sense ofcombined contributions to the tidal dissipation from Uranus + from satellite)yields the really observed magnitudes of decelerations for semi-major axises ofall the satellites of Uranus. Meanwhile, internal heat generation effects inthe satellites (due to tidal dissipation effect) are much more than those whichdefinitely take place in the Uranus, excepting the case of Ariel.

About influence of differential rotation in convection zone of gaseous or fluid giant Planet (Uranus) onto the parameters of orbits of satellites