The long term time evolution of tidal dwarf satellite galaxies with two different initial densities orbiting a host galaxy that resembles the Milky Way has been studied using a large set of Newtonian N-Body simulations .
From the simulations two maps of the orbital conditions that lead to quasi-equilibrium objects were constructed .
It has been found that several orbits of the satellites allow for the existence , for about 1 Gyr or more , of out-of-equilibrium bodies with high apparent mass-to-light ratios .
Within this framework the satellites in the quasi-stable phase reproduce the observed satellite properties for about 16 % of the orbit for high density progenitors , and for about 66 % for progenitors with lower densities An additional simulation for a single satellite with initial mass of 10 ^ { 7 } M _ { \odot } and Plummer radius of 0.15 kpc leads to remnants in the quasi-equilibrium phase that simultaneously reproduce remarkably well the observational quantities of the UFDGs of the Milky Way .
This satellite in the quasi-stable phase reproduces the observed satellite properties for about 42 % of the orbit .
The results suggest that a fraction of the observed satellites could plausibly be galaxies without dark matter that have true M/L ratios much lower than those measured .
The inflated M/L ratios arise because they are observed at the right time , along the right orbit and during the quasi-equilibrium phase of their evolution .
This is a viable explanation for the high M/L ratios observed in all satellites as long as the satellites are preferentially on certain orbits and are observed at certain times .
This could arise within the TDG scenario if all satellites are created at the same time along a few specific orbits that are particularly susceptible to the quasi-equilibrium phase .