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(Referência obtida automaticamente do Web of Science, por meio da informação sobre o financiamento pela FAPESP e o número do processo correspondente, incluída na publicação pelos autores.)

Dynamical evolution of the Cybele asteroids

Texto completo
Carruba, V. [1] ; Nesvorny, D. [2] ; Aljbaae, S. [1] ; Huaman, M. E. [1]
Número total de Autores: 4
Afiliação do(s) autor(es):
[1] Univ Estadual Paulista, UNESP, Grp Dinam Orbital & Planetol, BR-12516410 Guaratingueta, SP - Brazil
[2] Southwest Res Inst, Dept Space Studies, Boulder, CO 80302 - USA
Número total de Afiliações: 2
Tipo de documento: Artigo Científico
Fonte: Monthly Notices of the Royal Astronomical Society; v. 451, n. 1, p. 244-256, JUL 21 2015.
Citações Web of Science: 21

The Cybele region, located between the 2J:-1A and 5J:-3A mean-motion resonances, is adjacent and exterior to the asteroid main belt. An increasing density of three-body resonances makes the region between the Cybele and Hilda populations dynamically unstable, so that the Cybele zone could be considered the last outpost of an extended main belt. The presence of binary asteroids with large primaries and small secondaries suggested that asteroid families should be found in this region, but only relatively recently the first dynamical groups were identified in this area. Among these, the Sylvia group has been proposed to be one of the oldest families in the extended main belt. In this work we identify families in the Cybele region in the context of the local dynamics and non-gravitational forces such as the Yarkovsky and stochastic Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effects. We confirm the detection of the new Helga group at similar or equal to 3.65 au, which could extend the outer boundary of the Cybele region up to the 5J:-3A mean-motion resonance. We obtain age estimates for the four families, Sylvia, Huberta, Ulla, and Helga, currently detectable in the Cybele region, using Monte Carlo methods that include the effects of stochastic YORP and variability of the solar luminosity. The Sylvia family should be T = 1220 +/- 40 Myr old, with a possible older secondary solution. Any collisional Cybele group formed prior to the Late Heavy Bombardment would have been most likely completely dispersed in the jumping Jupiter scenario of planetary migration. (AU)

Processo FAPESP: 14/06762-2 - Famílias de asteroides em ressonâncias seculares
Beneficiário:Valerio Carruba
Modalidade de apoio: Auxílio à Pesquisa - Regular