ner_tags: O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O
tokens: of three stellar half-mass radii at infall on the individual orbits compared to the isolated run as a function of the central dark matter density slope at infall infall . The different initial dark matter density slope also affects the stellar mass-loss, since the dark matter acts as shield for the stars. In Fig. 16 , we plot the mass-loss as defined in Fig. 15 as function of the initial dark matter profile density slope but this time for stars and dark matter. In order to avoid a too crowded plot, we only show results for orbitIV , which is the most disruptive orbit for which all five satellites still have a well-defined centre. Figure 16. Dark matter (dots) and stellar (stars) mass enclosed in a constant sphere with a radius of three stellar half-mass radii at infall on orbitIV compared to the isolated run as a function of the central dark matter density slope at infall infall . In general stars are more resilient to tidal forces than dark matter, and this is due to their smaller spatial extent and larger stellar density; for example satIII is able to retain 40percent of its stars while it is practically totally stripped of dark matter. Nevertheless there is still a correlation between the stellar mass-loss and the initial dark matter slope. An exception to this relation seems to be given by satI , which has a very strong mass-loss both in the stellar and dark matter components despite having a similar infall as satIII . This is due to the different slope for the stellar density profiles between satI and satIII , while the first satellite has a slope of 1.80 (again evaluated between 1 and 2percent of the virial radius), the stellar slope for satIII (and all the other satellites) it is close to 3.0. This difference in stellar slope is most likely related to a major merger event that occurred for satI shortly before redshift one and strongly reshuffled the stellar particle orbits. Finally, we note that some satellites (especially satI ) are left at z 0 with practically no dark matter in their central region, where they are fully stellar dominated, resembling more an extended globular cluster than a dwarf galaxy, we plan to look more into this issue in a forthcoming paper. 4 DISCUSSION AND CONCLUSIONS This work is the second of a series of papers in which we are trying to understand the formation and evolution of the smallest galaxies in the universe. In the first paper ( Paper I ), we presented a series of 27 cosmological simulations of haloes in the mass range 510 8 to 10 10 , these simulations were run till z 1 and aimed to describe the properties of satellite galaxies before accretion. In this second paper, we used a subsample of these cosmological simulations as initial conditions for a series of binary hydrodynamical simulations (satellite host) with the goal of understanding the effects of accretion and environment on satellite galaxies. More specifically, we used a total of seven haloes (five luminous and two dark) with a virial mass