[en] It is shown, that the angular moment is transferred from the outer massive ring to inner ringe by dust component drifted across the Uranian rings. It is the angular moment transfer that provide the stability of the inner rings regarding the aerodynamical drag

[en] We report on the numerically integrated orbits for the nine outer Uranian satellites. The orbits are calculated based on fits to the astrometric observations for the period from 1984 to 2006. The results include the state vectors, post-fit residuals, and mean orbital elements. We also assess the accuracy of the orbital fits and discuss the need for future measurements.

No abstract available

[en] Uranus is unique among the solar planets, because its spin axis shows a tilt of 90deg and therefore it lies almost in its orbital plane. It is proposed that this peculiarity of its rotation is due to a tidal encounter of proto-uranus with a massive passing planetary body in the early solar system, that may still be detected as the tenth planet. (author). 7 refs

[en] Mutual position of Uranus rings and low order resonances (1:2,2:3,3:4,4:5,1:3,3:5) from ten new satellites is investigated. It is shown that ring distribution is not random: they are primarily located at 125-250 km distance from resonances. Statistical value of ring concentration at the given distances from resonances is 3.5 σ. This regularity confirms the ring formation model at the resonance spiral wave boundary in the Uranus protodisc. In this case the coefficient of correlation between the ring number and lower order resonance number in each 1000-km interval achieves 0.84±0.08

[en] The Uranus planet system described popularly, basic characteristics of the planet and its satellites are presented. Particular attention is paid to dust rings of the Uranus discovered in 1977. The models of the planet formation and structure, satellites and rings are presented in brief

[en] The problem of ring structure in the solar system planets is discussed. Three instabilities of planetary disks are considered. Jeans instability, dissipative instability and instability of negative diffusion. The instabilities result in the formation of narrow rings. Wide rings formed in the process of accretion instability development

[en] The results of photometric observations of the occulation of BD-19⁰4222 by Uranus on April 26, 1981 from two stations in India conform with the model proposed by Elliot et al. (1981). (Auth.)

[en] Two photoelectric records of the occultation event on 10 March, 1977, obtained by two 102-cm-aperture telescopes, spaced 1500 km apart, are critically analysed and indications of a complex structure of distribution of occulting material surrounding the planet are obtained. The results confirm the existence of a very shallow broad ring system with local condensation lanes of narrow and intermediate widths. A system of numerous thin rings are also present around the planet in the equatorial plane. (Auth.)

No abstract available