Volume 536, December 2011
|Number of page(s)||16|
|Section||Planets and planetary systems|
|Published online||07 December 2011|
Effects of the planetary migration on some primordial satellites of the outer planets⋆
I. Uranus’ case
1 Universidade Estadual Paulista, IGCE-DEMAC, Caixa Postal 178, CEP 13.500-970 Rio Claro (São Paulo), Brasil
e-mail: email@example.com; firstname.lastname@example.org
2 Observatório Nacional, Rua General Cristino 77, CEP 20921-400 Rio de Janeiro, RJ, Brasil
3 Universidade de São Paulo, IAG-USP, Rua do Matão 1226, CEP 05508-090, Cidade Universitária, São Paulo, Brasil
Received: 25 April 2010
Accepted: 12 September 2011
Context. During the first hundred million years after the formation of our solar system, the four giant planets are believed to have migrated significantly (by up ≈ 20 AU). The current scenario and dynamics of the satellites of these planets must be the result of both the initial conditions of their formation and this early extensive migrational episode.
Aims. We examine the effects of the migration on the primordial satellites of Uranus.
Methods. We use the Nice model to generate templates for the evolution of the four giant planets and record the time history of these planets and important close encounters. The satellites are then added to Uranus and these objects are integrated according to the dynamics stored in the templates.
Results. We show that Oberon is the outermost regular satellite of Uranus that is able to resist the close encounters during the extensive migrational episode. Some theories predict that Uranus’ satellites can form out to a 57 RU distance from the planet, but we show that even those at ≈ 27 RU from the planet cannot support the instabilities that appeared during migration. Close objects, such as the current regular satellites of Uranus, can survive quite stably and we are able to place some constraints on the masses of the planetesimals that have close encounters. For instance, if an object with mass ≥ 10-9 M⊙ approaches at distances ≲ 23 RU from Uranus, the regular satellites can be destabilized or their eccentricities or inclinations excited to some non-compatibles values. We also find that planet-planetesimal close encounters can generate capture. In this way, we present a promising means of explaining the origin of the irregular satellites of Uranus. The importance of the oblateness of the planet, and the Sun for just-captured planetesimals is also shown.
Key words: celestial mechanics / planets and satellites: general / planets and satellites: individual: Uranus
Appendix B is available in electronic form at http://www.aanda.org
© ESO, 2011
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