Dynamical evolution of the Cybele asteroids

• Published in: Monthly notices of the Royal Astronomical Society Vol. 451; no. 1; pp. 244 - 256
• Main Authors: Carruba, V., Nesvorný, D., Aljbaae, S., Huaman, M. E.
• Format: Journal Article
• Language: English
• Published: London Oxford University Press 21.07.2015; Oxford University Press (OUP): Policy P - Oxford Open Option A
• Subjects: Asteroids; Astronomy; Astrophysics; Belts; Density; Gravity; Jupiter (planet); Luminosity; Monte Carlo methods; Physics; Stochastic models; Stochasticity; Symbols; minor planets, asteroids: individual: Cybele; celestial mechanics; minor planets, asteroids: general; asteroids: individual: Cybele -celestial mechanics; asteroids: general Minor planets; Minor planets
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1093/mnras/stv997

The Cybele region, located between the 2J:-1A and 5J:-3A mean-motion resonances, is adjacent and exterior to the asteroid main belt. An increasing density of three-body resonances makes the region between the Cybele and Hilda populations dynamically unstable, so that the Cybele zone could be considered the last outpost of an extended main belt. The presence of binary asteroids with large primaries and small secondaries suggested that asteroid families should be found in this region, but only relatively recently the first dynamical groups were identified in this area. Among these, the Sylvia group has been proposed to be one of the oldest families in the extended main belt. In this work we identify families in the Cybele region in the context of the local dynamics and non-gravitational forces such as the Yarkovsky and stochastic Yarkovsky–O'Keefe–Radzievskii–Paddack (YORP) effects. We confirm the detection of the new Helga group at ≃3.65 au, which could extend the outer boundary of the Cybele region up to the 5J:-3A mean-motion resonance. We obtain age estimates for the four families, Sylvia, Huberta, Ulla, and Helga, currently detectable in the Cybele region, using Monte Carlo methods that include the effects of stochastic YORP and variability of the solar luminosity. The Sylvia family should be T = 1220 ± 40 Myr old, with a possible older secondary solution. Any collisional Cybele group formed prior to the Late Heavy Bombardment would have been most likely completely dispersed in the jumping Jupiter scenario of planetary migration.