Abstract
Secular perturbations of fictitious satellites that are initially circular and in the equatorial plane of Uranus are discussed. Satellites located in the region where the solar perturbation is dominant become highly eccentric and inclined with respect to the equator, and have a possibility to collide with Uranus. Satellites located in the region where the oblateness perturbation is dominant keep the original eccentricity and the inclination. A scenario of a possible extinction of outer satellites of Uranus is also discussed.
This is a preview of subscription content, log in via an institution to check access.
Similar content being viewed by others
References
French, R.G., Elliot, J.L., Levine, S.E.: 1986, Icarus 67, 134.
Hori, G.: 1979, in Nomura, T., ed(s)., 12th ISAS Lunar and Planetary Symposium, Institute of Space and Astronautical Science, Tokyo, 166–170.
Kinoshita, H.: 1972, Publ. Astron. Soc. Japan 24, 423.
Kinoshita, H.: 1990, submitted to Celestial Mechanics.
Kozai, Y.: 1962, Astron. J. 67, 591.
Author information
Authors and Affiliations
Rights and permissions
About this article
Cite this article
Kinoshita, H., Nakai, H. Secular perturbations of fictitious satellites of uranus. Celestial Mech Dyn Astr 52, 293–303 (1991). https://doi.org/10.1007/BF00048489
Received:
Accepted:
Issue Date:
DOI: https://doi.org/10.1007/BF00048489