Orbits of distant satellites of stars

Planar motion of point mass in the field of a point mass (a star) and the Galaxy was studied numerically. The tidal (quadratic) approximation for the galactic potential was accepted. The equations of motion were integrated for the time interval equal to $60/\sqrt{A(A-b)}$ ($A$, $B$ are Oort's coefficients). A particle was considered as escaping if its distance from the star exceeded two distances of the libration points. It was found that osculating eccentricities of remaining particles could be decreasing systematically or almost constant. Table 1 shows dependence of orbit types on initial conditions.