Busca avançada
Ano de início
(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.)

Characterizing the original ejection velocity field of the Koronis family

Texto completo
Carruba, V. [1, 2] ; Nesvorny, D. [2] ; Aljbaae, S. [1]
Número total de Autores: 3
Afiliação do(s) autor(es):
[1] Univ Estadual Paulista, UNESP, Grp Dinam Orbital & Planetol, BR-12516410 Guaratingueta, SP - Brazil
[2] Southwest Space Res Inst, Dept Space Studies, 1050 Walnut St, Boulder, CO 80302 - USA
Número total de Afiliações: 2
Tipo de documento: Artigo Científico
Fonte: ICARUS; v. 271, p. 57-66, JUN 1 2016.
Citações Web of Science: 7

An asteroid family forms as a result of a collision between an impactor and a parent body. The fragments with ejection speeds higher than the escape velocity from the parent body can escape its gravitational pull. The cloud of escaping debris can be identified by the proximity of orbits in proper element, or frequency, domains. Obtaining estimates of the original ejection speed can provide valuable constraints on the physical processes occurring during collision, and used to calibrate impact simulations. Unfortunately, proper elements of asteroids families are modified by gravitational and non-gravitational effects, such as resonant dynamics, encounters with massive bodies, and the Yarkovslcy effect, such that information on the original ejection speeds is often lost, especially for older, more evolved families. It has been recently suggested that the distribution in proper inclination of the Koronis family may have not been significantly perturbed by local dynamics, and that information on the component of the ejection velocity that is perpendicular to the orbital plane (v(W)), may still be available, at least in part. In this work we estimate the magnitude of the original ejection velocity speeds of Koronis members using the observed distribution in proper eccentricity and inclination, and accounting for the spread caused by dynamical effects. Our results show that (i) the spread in the original ejection speeds is, to within a 15% error, inversely proportional to the fragment size, and (ii) the minimum ejection velocity is of the order of 50 m/s, with larger values possible depending on the orbital configuration at the break-up. (C) 2016 Elsevier Inc. All rights reserved. (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
Linha de fomento: Bolsas no Brasil - Pós-Doutorado
Processo FAPESP: 14/24071-7 - Evolução dinâmica de famílias de asteroides
Beneficiário:Valerio Carruba
Linha de fomento: Bolsas no Exterior - Pesquisa