Advanced search
Start date
(Reference retrieved automatically from Web of Science through information on FAPESP grant and its corresponding number as mentioned in the publication by the authors.)

Characterizing the original ejection velocity field of the Koronis family

Full text
Carruba, V. [1, 2] ; Nesvorny, D. [2] ; Aljbaae, S. [1]
Total Authors: 3
[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
Total Affiliations: 2
Document type: Journal article
Source: ICARUS; v. 271, p. 57-66, JUN 1 2016.
Web of Science Citations: 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)

FAPESP's process: 13/15357-1 - Long-term effect of “The masses (ánd their uncertainties) of large asteroids ón “The orbital evolution of terrestrial planetes ánd minor bodies
Grantee:Safwan Aljbaae
Support type: Scholarships in Brazil - Post-Doctorate
FAPESP's process: 14/24071-7 - Dynamical evolution of asteroid families
Grantee:Valerio Carruba
Support type: Scholarships abroad - Research