The Eos family halo

Abstract

We study K-type asteroids in the broad surroundings of the Eos family because they seem to be intimately related, according to their colours measured by the Sloan Digital Sky Survey. Such `halos' of asteroid families have been rarely used as constraints for dynamical studies to date. We explain its origin as bodies escaping from the family `core' due to the Yarkovsky semimajor-axis drift and interactions with gravitational resonances, mostly with the 9/4 mean-motion resonance with Jupiter at 3.03 AU. Our N-body dynamical model allows us to independently estimate the age of the family 1.5 to 1.9 Gyr. This is approximately in agreement with the previous age estimate by Vokrouhlický et al. (2006) based on a simplified model (which accounts only for changes of semimajor axis). We can also constrain the geometry of the disruption event which had to occur at the true anomaly f =~ 120 to 180 deg.

submitted to Icarus

References in corpus (1)

• The Size Distributions of Asteroid Families in the SDSS Moving Object Catalog 4

Cited by in corpus (9)

• Main Belt Asteroids with WISE/NEOWISE: Near-Infrared Albedos
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• Yarkovsky V-shape identification of asteroid families
• Spin states of asteroids in the Eos collisional family
• Hektor - an exceptional D-type family among Jovian Trojans
• Stability of Jovian Trojans and their collisional families
• Asteroid cratering families: recognition and collisional interpretation
• Asteroid migration due to the Yarkovsky effect and the distribution of the Eos family
• Asteroid spin-states of a 4 Gyr collisional family