Physics
Scientific paper
Sep 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994sosyr..28..152s&link_type=abstract
Solar System Research, Vol. 28, No. 2, p. 152 - 162
Physics
3
Minor Planets: Orbital Evolution, Minor Planets: Radiation Pressure
Scientific paper
A method of numerical investigation of the evolution of the orbital elements of an asteroid and the parameters of its motion about its center of mass due to external perturbing forces is described. The method is based on numerical averaging of the right sides of differential equations for the osculating orbital elements and the analogous parameters of motion about the center of mass based on the Euler-Poinsot rotational motion and the Keplerian orbital motion using theoretical numerical quadrature equations. Examples are given of numerical integration of averaged equations in the case in which light pressure and gravitational torque exerted on an asteroid by the Sun take the role of the perturbation. It is shown that for ≍10 m asteroids, the main factor determining the evolution of the parameters of their rotational motion is the light pressure torque. The characteristic time of influence of light pressure on an asteroid's rotational motion is considerably shorter than the analogous time for its orbital motion.
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