Non-gravitational perturbations and evolution of the asteroid main belt

Details Non-gravitational perturbations and evolution of the asteroid main belt Non-gravitational perturbations and evolution of the asteroid main belt

Feb 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005dpps.conf..145v&link_type=abstract

Dynamics of Populations of Planetary Systems, Proceedings of IAU Colloquium #197, held 31 August - 4 Spetember, 2004 in Belgrade

Physics

1

Minor Planets, Asteroids, Interplanetary Medium, Radiation Mechanisms: Thermal.

Scientific paper

Gravity is the most important force to affect the motion of bodies in the Solar system. At small sizes, however, additional forces must be taken into account to explain fine details of their translational and rotational motion, as well as parameters of their populations. This is because the strength of the non-gravitational perturbations typically increases as ≃ 1/D toward small sizes D. The principal perturbation acting on macroscopic main-belt bodies (sizes up to several kilometers for timescales of about billion years) is due to the anisotropic thermal re-radiation of the absorbed sunlight. In orbital dynamics this is known as the Yarkovsky effect, while in rotational dynamics the same physical phenomenon is called the YORP (Yarkovsky-O'Keefe-Radzievskii-Paddack) effect. We review the main observational implications of the Yarkovsky/YORP effects as understood and evidenced today.

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