hydrodynamical simulations of dwarf-main host interaction in which a diffuse gaseous halo consistent with observational constraints is added to the dark halo of the main host ([@2006MNRAS.369.1021M]; [@2010HiA....15..193M]).

These studies established tidal stirring as a major mode of morphological evolution of dwarf galaxies, turning them from faint rotationally supported disks into even fainter pressure supported spheroidals, thus providing a natural explanation for the morphology-density relation ubiquitously observed in galaxy groups, including our own Local Group ([@1999AAS...195.0803G]).

Direct tidal heating as well as indirect heating stemming from bar and buckling instabilities triggered by tidal shocks have been both shown to play a role in tidal stirring, although the latter requires initial disks with mass-to-light ratios at the upper end of those observed in dwarf galaxies ([@2001ApJ...547L.123M]; [@2011ApJ...726...98K]). These works also determined that ram pressure mass removal aided by tidal shocks can rapidly remove the gas content of satellites explaining why dSphs are devoid of gas and why they can have very high mass-to-light ratios.

Recently the effect of the dark matter density profile of dwarf galaxies on tidal stirring has been studied, motivated by the new findings of cosmological hydrodynamical simulations of field dwarf galaxy formation which have shown that feedback 