from supernovae and massive stars can turn the cuspy halos predicted by $\Lambda$CDM into halos with shallower inner density slopes ($\gamma$ in \[0.3, 0.7\] range), depending on the star formation rate achieved in the galaxy ([@2010Natur.463..203G]; [@2012MNRAS.421.3464P]; [@2014ApJ...792...99S]; [@2012MNRAS.422.1231G]; [@2013MNRAS.431.1220D]; [@2015MNRAS.446.1140T]). There have also been attempts to show the existence of this effect specifically for dwarf galaxy satellites, albeit in this case resolution is a potential issue ([@2013ApJ...765...22B]). [@2012ApJ...751L..15L] and [@2013ApJ...764L..29K] have thus updated the previous tidal stirring simulations by carrying out N-Body simulations in which disky dwarf galaxies have shallower dark matter profiles as those arising in the cosmological hydro simulations, and have checked results against varying resolution. They have found that the transformation by tidal stirring is enhanced significantly when a shallower density profile is adopted ($\gamma =0.2$ or $0.6$). They have also found that, since mass loss is also enhanced, remnants of dwarfs with shallow dark matter profiles can evolve into very faint objects such as Ultra Faint Dwarfs ([@2012ApJ...751L..15L]). The enhanced mass loss and transformation follow from the lower binding energy and more impulsive dynamical response of the system in the case of objects with a shallower halo profile.

However, these recent simulations, exactly like those 