An Analysis of the Region of the Phocaea Dynamical Family

Details An Analysis of the Region of the Phocaea Dynamical Family An Analysis of the Region of the Phocaea Dynamical Family

Sep 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009dps....41.2704c&link_type=abstract

American Astronomical Society, DPS meeting #41, #27.04

Astronomy and Astrophysics

Astronomy

Scientific paper

In this work we conduct an analysis of the Phocaea dynamical family region. We obtain families and clumps in the space of proper elements and frequencies, study the taxonomy of the asteroids for which this information is available, analyze the albedo and absolute magnitude distribution of objects in the area, obtain a preliminary estimate of the family age, study the cumulative size distribution and collision probabilities of asteroids in the region, and obtain dynamical maps of averaged elements and Lyapunov times for grids of objects in the area.
Among our results, we identified the first clump only observable in the frequency domain, around (6246) Komurotoru, obtained a higher limit for the possible age of the Phocaea family of 2.2 Byr, identified a class of Phocaea members on Mars-crossing orbits characterized by low Lyapunov times, and showed that an apparently stable region on timescales of 20 Myr near the g-g6 secular resonance is chaotical. The Phocaea dynamical group seems to be a real S-type collisional family, formed up to 2.2 Byr ago, whose members with large semi-major axis have been dynamically eroded by the interaction with the local web of mean-motion and secular resonances.
Studying the long-term stability of orbits in the chaotic regions and the stability of families and clumps identified in this work remain challenges for future works.
This work has been supported by the FAPESP and CNPq funding agency.

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