The program MONS-EPH is constructed in such a way that any satellite motion model may be used and a corresponding computing program may be included into the program system. On the current stage (version 1.01) of the program development we have realized some simplified theories for almost all satellites. For some satellites we have realized the most adequate theories. The following explications indicate the adopted theories.
a. Mars satellites - Phobos and Deimos. The motion models are the Keplerian osculating orbits with the mean elements according to (Emelyanov et al. 1993). Although we have an adequate model realization which was fitted to all available observations (Emelyanov et al. 1993) and this model may be included.
b. Jupiter satellites. Galilean satellite motion models are founded on the work of Lieske (1977) with constants corrected by Arlot (1982). This is the most adequate theory of the Galilean satellite motion by now. For the rest satellites of Jupiter the osculating Keplerian orbits are realized with mean elements according to various papers. These models are approximate.
c. Saturn satellites. For the major satellites of Saturn (Mimas, Enceladus, Tethys, Dione, Rhea, Titan, Iapetus) the motion theories published by Harper and Taylor (1993) are used. For Hyperion the theory published in the paper of Taylor et al. (1987) is used. These theories are of the most precise and adequate ones. The motion model of Phoebe is taken as a Keplerian orbit with constant elements according to the paper by Bykova and Shikhalev (1982). For the eight faint satellite of Saturn the motion model is taken as a Keplerian orbit with constant elements according to Synnot et al. (1981).
d. Uranus satellites. For five major satellites the precise and adequate motion models are realized according to the work by Laskar and Jacobson (1987). For ten faint satellites the results from Owen end Synnott (1987) are used.
e. Neptune satellites. The motion model for Triton and Nereid is taken as osculating Keplerian orbit with mean elements from Jacobson (1990). For six faint satellites the results from Owen et al. (1991) are used.
f. The system Pluto-Charon. A separate program was constructed to precalculate the circumstances of mutual phenomena in this system. Mean elements are taken from Tholen et al. (1987).