ИСТИНА

Quasi-capture or temporary capture of a small body (asteroid, planetesimal and so on) by planet can be explained with so called stickiness phenomenon. The stickiness phenomenon occurs when an orbit positioning in the immediate vicinity of the last invariant torus remains rather close to this torus for long time before leaving it into the chaotic sea. It is a well known fact that stickiness phenomenon takes place due to the presence of the cantori which are the remain parts of the invariant tori. These tori are destroyed by the perturbation and form the Cantor sets of points on the section surface. A cantorus forms only a partial barrier to chaotic orbits, which can penetrate into and abandon the vicinity of the last invariant torus passing through the gaps of the cantorus. The basic way of temporary capture investigation is intensive numerical simulation, which provides the following information as classification of quasi-capture orbits and distribution of their initial values. This approach does not use the structure of periodic solution and possible position of cantori. In contrary we propose to investigate the stickiness phenomenon in the vicinity of stability islands of the direct and retrograde families of satellite periodic orbits in planar Hill problem. This problem is an effective model using for investigation of satellite dynamic. The equations of motion of Hill problem have the only first integral and they are invariant under discrete group of phase space transformations with reverse of time. With the help of numerical simulation some stickiness regions were found out in Hill problem. These regions are placed in the outer space of last invariant curve and possess trajectories, which make more then 105 revolutions around the origin. Due to the time-reversal symmetry of equations of motion one can state that these trajectories have penetrated earlier into the stickiness region and stay there for a long time. The contemporary database of natural satellites of Solar system’s giant planets were used from the Natural Satellite Data Center of IMCCE, Paris and SAI, Moscow and from database of NASA JPL. The main parameters of the satellite orbits such as semi-major axis, eccentricity and orbit inclination were computed into the corresponding Hill unit of length equals to , where is the ratio of the mass of the planet to the total mass of Sun and the planet, is the semi-major axis of the planet's orbit. We have checked parameters of 59 Jupiter's outer satellites, 38 outer Saturn's outer satellites, 9 Uranus' outer satellites and 5 Neptune's outer satellites. There was found only one Jupiter's satellite S/2003 J2, which orbital motion is near the inner boundary of stability island around the family f of retrograde satellite orbits.