CAOSP abstracts, Volume: 48, No.: 2, year: 2018

Abstract: This paper describes a numerical simulation model of motion of moonlets in binary and multiple asteroid systems. Gravitational accelerations produced by the primary body, its moonlets, the Sun, the Moon, and eight major planets are accounted for in this model. The asymmetry of the primary and the effects of solar radiation pressure on the moons in asteroid systems are also factored in. To run the numerical simulation, we adopted the orbital state vectors of celestial bodies from the numerical theory. Using Keplerian orbital elements of the primaries of asteroid systems, we determined their heliocentric positions. Differential equations of motion of celestial bodies in asteroid systems were solved in the asteroid-centric Cartesian reference frame by the Everhart 15th-order method of integration. The verification and validation of the simulation model have been performed for three asteroid systems, namely (136617) 1994 CC and (87) Sylvia, which belong to the near-Earth and main belt populations, respectively, and (136108) Haumea, which is a trans-Neptunian object. These are three asteroid systems of almost 300 small Solar-system bodies with discovered moons which are known to date. All six Keplerian orbital elements determined with reasonable accuracy are available for all asteroid moons.