PECULIAR EUPHROSYNE

Autor(es)

Carruba, V. ^[1] ; Aljbaae, S. ^[1] ; Souami, D. ^{[2, 3]}

Afiliação do(s) autor(es)

^[1] Univ Estadual Paulista, UNESP, Grp Dinam Orbital & Planetol, BR-12516410 Guaratingueta, SP - Brazil

^[2] Univ Namur, Dept Math, Namur Ctr Complex Syst, NAXYS, B-5000 Namur - Belgium

^[3] Univ Paris 06, F-75005 Paris - France

• Tipo de documento: Artigo Científico
• Fonte: ASTROPHYSICAL JOURNAL; v. 792, n. 1 SEP 1 2014.
• Citações Web of Science: 11

Resumo

The asteroid (31) Euphrosyne is the largest body of its namesake family, and it contains more than 99% of the family mass. Among large asteroid families, the Euphrosyne group is peculiar because of its quite steep size-frequency distribution (SFD), significantly depleted in large-and medium-sized asteroids (8 < D < 12 km). The current steep SFD of the Euphrosyne family has been suggested to be the result of a grazing impact in which only the farthest, smallest members failed to accrete. The Euphrosyne family is, however, also very peculiar because of its dynamics: near its center it is crossed by the nu(6) = g - g(6) linear secular resonance, and it hosts the largest population (140 bodies) of asteroids in nu(6) antialigned librating states (or Tina-like asteroids) in the main belt. In this work we investigated the orbital evolution of newly obtained members of the dynamical family, with an emphasis on its interaction with the nu(6) resonance. Because of its unique resonant configuration, large-and medium-sized asteroids tend to migrate away from the family orbital region faster than small-sized objects, which were ejected farther away from the family center. As a consequence, the SFD of the Euphrosyne family becomes steeper in time with a growing depletion in the number of the largest family members. We estimate that the current SFD could be attained from a typical, initial SFD on timescales of 500 Myr, consistent with estimates of the family age obtained with other independent methods. (AU)

• Processo FAPESP: 13/15357-1 - Efeito a longo prazo das massas (e sua incertidão) dos asteroides massivos sobre a evolução orbital de planetas terrestres e corpos menores.
• Beneficiário: Safwan ALJBAAE
• Modalidade de apoio: Bolsas no Brasil - Pós-Doutorado
• Processo FAPESP: 14/06762-2 - Famílias de asteroides em ressonâncias seculares
• Beneficiário: Valerio Carruba
• Modalidade de apoio: Auxílio à Pesquisa - Regular
• Processo FAPESP: 11/19863-3 - Mobilidade orbital causada por encontros próximos com mais de um asteroide massivo
• Beneficiário: Valerio Carruba
• Modalidade de apoio: Auxílio à Pesquisa - Regular