| Texto completo | |
| Autor(es): |
de Sousa, Rafael Ribeiro
[1, 2]
;
Gomes, Rodney
[3]
;
Morbidelli, Alessandro
[2]
;
Neto, Ernesto Vieira
[1]
Número total de Autores: 4
|
| Afiliação do(s) autor(es): | [1] Sao Paulo State Univ, UNESP, Campus Guaratingueta, BR-12516410 Guaratingueta, SP - Brazil
[2] Univ Cote Azur, Observ Cote Azur, CNRS, Lab Lagrange, UMR7293, Blvd Observ, F-06304 Nice 4 - France
[3] Observ Nacl, Rua Gen Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ - Brazil
Número total de Afiliações: 3
|
| Tipo de documento: | Artigo Científico |
| Fonte: | ICARUS; v. 334, p. 89-98, DEC 2019. |
| Citações Web of Science: | 1 |
| Resumo | |
The link between the dynamical evolution of the giant planets and the Kuiper Belt orbital structure can provide clues and insight about the dynamical history of the Solar System. The classical region of the Kuiper Belt has two populations (the cold and hot populations) with completely different physical and dynamical properties. These properties have been explained in the framework of a sub-set of the simulations of the Nice Model, in which Neptune remained on a low-eccentricity orbit (Neptune's eccentricity is never larger than 0.1) throughout the giant planet instability (NesvornY 2015a,b). However, recent simulations (Gomes et al., 2018) have showed that the remaining Nice model simulations, in which Neptune temporarily acquires a large-eccentricity orbit (larger than 0.1), are also consistent with the preservation of the cold population (inclination smaller than 4 degrees), if the latter formed in situ. However, the resulting a cold population showed in many of the simulations eccentricities larger than those observed for the real population. The purpose of this work is to discuss the dynamical effects on the Kuiper belt region due to an excited Neptune phase. We focus on a short period of time, of about six hundred thousand years, which is characterized by Neptune's large eccentricity and smooth migration with a slow precession of Neptune's perihelion. This phase was observed during a full simulation of the Nice Model (Gomes et al., 2018) just after the last jump of Neptune's orbit due to an encounter with another planet. We show that if selfgravity is considered in the disk, the precession rate of the particles longitude of perihelion `ay is slowed down, which in turn speeds up the cycle of (omega) over bar - (omega) over bar (N)(the subscript N referring to Neptune), associated to the particles eccentricity evolution. This, combined with the effect of mutual scattering among the bodies, which spreads all orbital elements, allows some objects to return to low eccentricities. However, we show that if the cold population originally had a small total mass, this effect is negligible. Thus, we conclude that the only possibilities to keep at low eccentricity some cold-population objects during a high-eccentricity phase of Neptune are that (i) either Neptune's precession was rapid, as suggested by Batygin et al. (2011) or (ii) Neptune's slow precession phase was long enough to allow some particles to experience a full secular cycle of (omega) over bar - (omega) over bar (N). (AU) | |
| Processo FAPESP: | 15/15588-9 - A estabilidade na evolução dinâmica do Sistema Solar via Modelo de Nice |
| Beneficiário: | Rafael Ribeiro de Sousa |
| Modalidade de apoio: | Bolsas no Brasil - Doutorado |
| Processo FAPESP: | 17/09919-8 - Um estudo da autogravidade do disco de planetesimais no Modelo de Nice e a formação dinâmica do cinturão de Kuiper |
| Beneficiário: | Rafael Ribeiro de Sousa |
| Modalidade de apoio: | Bolsas no Exterior - Estágio de Pesquisa - Doutorado |