Secular evolution of asteroid families: the role of Ceres

2016

Icarus

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In this work we explore dynamical perturbations induced by the massive asteroids Ceres and Vesta on main-belt asteroids through secular resonances. First we determine the location of the linear secular resonances with Ceres and Vesta in the main belt, using a purely numerical technique. Then we use a set of numerical simulations of fictitious asteroids to investigate the importance of these secular resonances in the orbital evolution of main-belt asteroids. We found, evaluating the magnitude of the perturbations in the proper elements of the test particles, that in some cases the strength of these secular resonances is comparable to that of known non-linear secular resonances with the giant planets. Finally we explore the asteroid families that are crossed by the secular resonances we studied, and identified several cases where the latter seem to play an important role in their post-impact evolution.

Section: Asteroid Familiesmentioning

confidence: 84%

Secular resonances with Ceres and Vesta

Tsirvoulis

2016

Icarus

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“…It is known that two largest objects in the asteroid belt, namely (1) Ceres and (4) Vesta may significantly perturb orbital motion of asteroids. The perturbing mechanisms include meanmotion resonances (Christou & Wiegert 2012), close encounters (Carruba, et al 2003) or secular resonances Novaković et al 2016). In Section 2.3, we concluded that the secular resonance − + − with asteroid Vesta is crossing the family.…”

Section: The Role Of Ceres and Vestamentioning

confidence: 86%

Analysis of the Karma asteroid family

Pavela

Monthly Notices of the Royal Astronomical Society

Carruba

et al. 2020

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The Karma asteroid family is a group of primitive asteroids in the middle part of the main belt, just at the outer edge of the 3J:1A mean-motion resonance. We obtained the list of the family members with 317 asteroids, and estimated that it was formed by the catastrophic disruption of a parent body that was between 34 and 41 km in diameter. Based on the V-shape method, age of the Karma family is estimated to be about 137 Myr. A detailed dynamical map of the region combined with numerical simulations allowed us to reconstruct the long-term dynamical evolution of the family, and to identify the mechanisms responsible for this evolution. The numerical simulations successfully reproduced the main features in the orbital distribution of the family members but also showed that some regions of the Karma family could be missing. A more detailed analysis revealed that these regions likely consist of very dark objects, fainter than absolute magnitude H=17, that have not yet been detected. Based on the obtained results, we concluded that magnitude-frequency distribution of family members up to H=16 mag is neither affected by dynamical erosion nor observational incompleteness, and therefore represents the result of collisional grinding of the original family population. Finally, we found that the Karma family have been supplying some asteroids to the near-Earth region via the 3J:1A resonance. Currently there should about 10 family members larger than 1 km in diameter, orbiting in the near-Earth space.

“…Regarding the interaction with ν 1C secular resonance, an interesting case for further study is the Seinajoki asteroid family. The family is also crossed by this resonance (Tsirvoulis and Novaković 2016), and its overall shape in the (a p , sin i p ) plane could be explained by the effects of the ν 1C resonance (Novaković et al 2016). However, although the perturbation caused by this resonance explains the overall shape of the Seinajoki, several smaller features remain unexplained.…”

Section: Long-term Dynamical Evolutionmentioning

confidence: 96%

“…The Astrid family members have an unusual orbital inclination distribution, the feature caused by an interaction of the family with the ν 1C nodal secular resonance with Ceres (Novaković et al 2016). Consequently, the observed distribution of the v W component of terminal ejection velocities is quite leptokurtic.…”

Section: Long-term Dynamical Evolutionmentioning

confidence: 98%

Asteroid families: properties, recent advances, and future opportunities

Vokrouhlický

Spoto

et al. 2022

Celest Mech Dyn Astron

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Collisions are one of the key processes shaping planetary systems. Asteroid families are outcomes of such collision still identifiable across our solar system. The families provide a unique view of catastrophic disruption phenomena and have been in the focus of planetary scientists for more than a century. Most of them are located in the main belt, a ring of asteroids between Mars and Jupiter. Here we review the basic properties of the families, discuss some recent advances, and anticipate future challenges. This review pays more attention to dynamic aspects such as family identification, age determination, and long-term evolution. The text, however, goes beyond that. Especially, we cover the details of young families that see the major advances in the last years, and we anticipate it will develop even faster in the future. We also discuss the relevance of asteroid families for water-ice content in the asteroid belt and our current knowledge on links between families and main-belt comets. query Please check the edit made in the article title.