Dynamic picture of the inner asteroid belt: implications for the density, size and taxonomic distributions of real objects

• Published in: Monthly notices of the Royal Astronomical Society Vol. 401; no. 4; pp. 2499 - 2516
• Main Authors: Michtchenko, T. A., Lazzaro, D., Carvano, J. M., Ferraz-Mello, S.
• Format: Journal Article
• Language: English
• Published: Oxford, UK Blackwell Publishing Ltd 01.02.2010; Wiley-Blackwell; Oxford University Press
• Subjects: Asteroids; Astronomy; Earth, ocean, space; Exact sciences and technology; minor planets; minor planets, asteroids; Spectrum analysis; minor planets, asteroids; Spectral method; minor planets; Mars planet; Sun; Spectral analysis; Secular resonance; Initial conditions; Neptune planet; Dynamics; Gravitational interactions; Asteroids; Test particles; Asteroid belt
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1111/j.1365-2966.2009.15825.x

In this paper, we construct a dynamic portrait of the inner asteroidal belt. We use information about the distribution of test particles, which were initially placed on a perfectly rectangular grid of initial conditions, after 4.2 Myr of gravitational interactions with the Sun and five planets, from Mars to Neptune. Using the spectral analysis method introduced by Michtchenko et al., the asteroidal behaviour is illustrated in detail on the dynamical, averaged and frequency maps. On the averaged and frequency maps, we superpose information on the proper elements and proper frequencies of real objects, extracted from the data base, AstDyS, constructed by Milani and Knežević. A comparison of the maps with the distribution of real objects allows us to detect possible dynamical mechanisms acting in the domain under study; these mechanisms are related to mean-motion and secular resonances. We note that the two- and three-body mean-motion resonances and the secular resonances (strong linear and weaker non-linear) have an important role in the diffusive transportation of the objects. Their long-lasting action, overlaid with the Yarkovsky effect, may explain many observed features of the density, size and taxonomic distributions of the asteroids.