Captura, permanência e escape de ressonâncias do Sistema Solar
Um estudo da autogravidade do disco de planetesimais no Modelo de Nice e a formaçã...
Texto completo | |
Autor(es): |
Deienno, Rogerio
[1, 2]
;
Izidoro, Andre
[3]
;
Morbidelli, Alessandro
[4]
;
Gomes, Rodney S.
[5]
;
Nesvorny, David
[2]
;
Raymond, Sean N.
[6]
Número total de Autores: 6
|
Afiliação do(s) autor(es): | [1] Inst Nacl Pesquisas Espaciais, Ave Astronautas 1758, BR-12227010 Sao Jose Dos Campos, SP - Brazil
[2] Southwest Res Inst, Dept Space Studies, 1050 Walnut St, Boulder, CO 80302 - USA
[3] Univ Estadual Paulista, Grp Dinam Orbital & Planetol, Av Dr Ariberto Pereira da Cunha 333, BR-12516410 Guaratingueta, SP - Brazil
[4] Univ Cote Azur, UMR7293, Lab Lagrange, Observ Cote Azur, CNRS, Blvd Observ, F-06304 Nice 4 - France
[5] Observ Nacl, Rua Gen Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ - Brazil
[6] Univ Bordeaux, Lab Astrophys Bordeaux, CNRS, B18N, Allee Geoffroy St Hilaire, F-33615 Pessac - France
Número total de Afiliações: 6
|
Tipo de documento: | Artigo Científico |
Fonte: | ASTROPHYSICAL JOURNAL; v. 864, n. 1 SEP 1 2018. |
Citações Web of Science: | 3 |
Resumo | |
The main asteroid belt (MB) is low in mass but dynamically excited. Here we propose a new mechanism to excite the MB during the giant planet (the ``Nice model{''}) instability, which is expected to feature repeated close encounters between Jupiter and one or more ice giants ({''}jumping Jupiter{''} or JJ). We show that, when Jupiter temporarily reaches a high-enough level of excitation, both in eccentricity and inclination, it induces strong forced vectors of eccentricity and inclination across the MB region. Because during the JJ instability Jupiter's orbit ``jumps{''} around, the forced vectors keep changing both in magnitude and phase throughout the whole MB region. The entire cold primordial MB is thus excited as a natural outcome of the JJ instability. The level of such an excitation, however, is typically larger than the current orbital excitation observed in the MB. We show that the subsequent evolution of the solar system is capable of reshaping the resultant overexcited MB to its present-day orbital state, and that a strong mass depletion (similar to 90%) is associated with the JJ instability phase and its subsequent evolution throughout the age of the solar system. (AU) | |
Processo FAPESP: | 16/19556-7 - Formação e Dinâmica Planetária: do Sistema Solar a Exoplanetas |
Beneficiário: | André Izidoro Ferreira da Costa |
Modalidade de apoio: | Bolsas no Brasil - Jovens Pesquisadores |
Processo FAPESP: | 14/02013-5 - Evolução orbital dos asteroides nos primeiros 700 MY do sistema solar |
Beneficiário: | Rogerio Deienno |
Modalidade de apoio: | Bolsas no Brasil - Pós-Doutorado |
Processo FAPESP: | 16/12686-2 - Formação e dinâmica planetária: do Sistema Solar a exoplanetas |
Beneficiário: | André Izidoro Ferreira da Costa |
Modalidade de apoio: | Auxílio à Pesquisa - Jovens Pesquisadores |