Asteroid families interacting with secular resonances

Abstract

Asteroid families are formed as the result of collisions. Large fragments are ejected with speeds of the order of the escape velocity from the parent body. After the family formation, the fragments' orbits evolve in the space of proper elements because of gravitational and non-gravitational perturbations, such as the Yarkovsky effect. Disentangling the contribution to the current orbital position of family members caused by the initial ejection velocity field and the subsequent orbital evolution is usually a difficult task. Among the more than 100 asteroid families currently known, some interact with secular resonances. Linear secular resonances occur when there is a commensurability between the precession frequency of the longitude of the pericenter (g) or of the longitude of node (s) of an asteroid and a planet, or a massive asteroid. The linear secular resonance most effective in increasing an asteroid eccentricity is the ${\nu }_6$, that corresponds to a commensurability between the precession frequency g of an asteroid and Saturn's $g_6$. Non-linear secular resonances involve commensurabilities of higher order, and can often be expressed as combinations of linear secular resonances. This is the case, for instance, of the $z_k=k(g-g_6)+(s-s_6)$ resonances. Asteroid families that are crossed by secular resonances are of particular interest in dynamical astronomy. First, they often provide a clear evidence of asteroid orbit evolution due to the Yarkovsky effect. Second, conserved quantities of secular dynamics can be used to set valuable constraints on the magnitude of the original ejection velocity field. Finally, by changing the value of inclination of family members nodal secular resonances with massive asteroids or dwarf planets can cause the i distribution to become more and more leptokurtic (i.e., more peaked and with larger tails than that of a Gaussian distribution).

arXiv comment27 pages, 15 figures, 1 table. Review paper accepted for publication in Planetary and Space Science

References in corpus (16)

• Asteroid families classification: exploiting very large data sets
• The Yarkovsky and YORP Effects
• Identification and Dynamical Properties of Asteroid Families
• Asteroid family ages
• On the V-type asteroids outside the Vesta family. I. Interplay of nonlinear secular resonances and the Yarkovsky effect: the cases of 956 Elisa and 809 Lundia
• On the Ages of Resonant, Eroded and Fossil Asteroid Families
• Constraints on the original ejection velocity fields of asteroid families
• Dynamical evolution of V-type asteroids in the central main belt
• Footprints of a possible Ceres asteroid paleo-family
• Secular resonances with Ceres and Vesta
• On the Erigone family and the $z_2$ secular resonance
• Origin and Sustainability of The Population of Asteroids Captured in the Exterior Resonance 1:2 with Mars
• On the Astrid asteroid family
• Secular evolution of asteroid families: the role of Ceres
• On the highly inclined $v_W$ leptokurtic asteroid families
• The Rafita asteroid family

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