Dynamical evolution of V-type photometric candidates in the outer main belt

Autor(es)

Huaman, M. E. ^[1] ; Carruba, V. ^[1] ; Domingos, R. C. ^[2]

Afiliação do(s) autor(es)

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

^[2] Univ Estadual Paulista, UNESP, BR-13874149 Sao Joao Da Boa Vista, SP - Brazil

• Tipo de documento: Artigo Científico
• Fonte: Monthly Notices of the Royal Astronomical Society; v. 444, n. 3, p. 2985-2992, NOV 1 2014.
• Citações Web of Science: 7

Resumo

V-type asteroids, characterized by two absorption bands at 1.0 and 2.0 mu m, are usually thought to be portions of the crust of differentiated or partially differentiated bodies. Most V-type asteroids are found in the inner main belt and are thought to be current or past members of the Vesta dynamical family. Recently, several V-type photometric candidates have been identified in the central and outer main belt. While the dynamical evolution of V-type photometric candidates in the central main belt has been recently investigated, less attention has been given to the orbital evolution of basaltic material in the outer main belt as a whole. Here, we identify known and new V-type photometric candidates in this region, and study their orbital evolution under the effect of gravitational and non-gravitational forces. A scenario in which a minimum of three local sources, possibly associated with the parent bodies of (349) Dembowska, (221) Eos, and (1459) Magnya, could in principle explain the current orbital distribution of V-type photometric candidates in the region. (AU)

• 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