Abstract
The dynamics of asteroids near mean motion resonances is considered in the paper. Results of study of orbital evolution of NEAs 2608 Seneca, 3103 Eger, 3838 Epona, 1994 RB, 1994 CB are presented. Equations of the motion of asteroids have been integrated numerically. In the process of numerical integration perturbations from planets and the Moon have been taken into account. The interval of time is ranging from −3000 to 3000 yr. Evolution of ensembles of 100 test particles with orbital elements nearby their nominal orbits has been considered for each object.
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