Analysis of the Karma asteroid family
arXiv:2012.02331 · doi:10.1093/mnras/staa3676
Abstract
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.
arXiv comment12 pages, 13 Postscript figures, accepted for publication in MNRAS
References in corpus (29)
- Main Belt Asteroids with WISE/NEOWISE I: Preliminary Albedos and Diameters
- Debiased orbit and absolute-magnitude distributions for near-Earth objects
- Asteroid families classification: exploiting very large data sets
- The Size Distributions of Asteroid Families in the SDSS Moving Object Catalog 4
- Asteroid family ages
- Families among high-inclination asteroids
- The Main Belt Comets and Ice in the Solar System
- A multi-domain approach to asteroid families identification
- On the Ages of Resonant, Eroded and Fossil Asteroid Families
- Asteroid Family Associations of Active Asteroids
- Constraints on the original ejection velocity fields of asteroid families
- Mineralogical Characterization of Baptistina Asteroid Family: Implications for K/T Impactor Source
- An automatic approach to exclude interlopers from asteroid families
- Chaotic Transport and Chronology of Complex Asteroid Families
- Portrait of Theobalda as a Young Asteroid Family
- Discovery of a young asteroid cluster associated with P/2012~F5 (Gibbs)
- Fragment properties from large-scale asteroid collisions: I: Results from SPH/N-body simulations using porous parent bodies and improved material models
- Asteroid families interacting with secular resonances
- Potential Themis Family Asteroid Contribution to the Jupiter-Family Comet Population
- Secular resonances with Ceres and Vesta
- Initial velocity V-shapes of young asteroid families
- A population of main belt asteroids co-orbiting with Ceres and Vesta
- Characterizing the original ejection velocity field of the Koronis family
- A Taxonomic Study of Asteroid Families from KMTNet-SAAO Multi-band Photometry
- Recent collisional jet from a primitive asteroid
- Secular evolution of asteroid families: the role of Ceres
- The Hoffmeister asteroid family
- Small Bodies Science with Twinkle
- P/2017 S5: Another Active Asteroid Associated with the Theobalda Family