i.e at $R < 300$ kpc, are classified as dwarf spheroidal galaxies (dSphs). They have fairly round stellar components with low or negligible rotation but relatively high velocity dispersions (; [@2012AJ....144....4M]). At the same time, nearly all of the dwarf galaxies located outside such radius and far from M31 are gas-rich dwarf irregular galaxies (dIrrs), which have ongoing or recent star formation, flattened disky shapes, and exhibit substantial rotational support ($v_{rot}/\sigma > 1$). The different spatial distribution of dwarf galaxy types is known as the morphology-density relation, and reflects an analogous effect seen in galaxy clusters and rich groups on larger mass scales ([@1980ApJ...236..351D]).

Environmental mechanisms have been often invoked to transform dIrrs into dSphs (; [@2012AJ....144....4M]). One of the mechanisms proposed to achieve such transformation is tidal stirring, namely the cumulative effect of repeated tidal shocks occurring near the pericenter of the eccentric orbits of satellites ([@2010HiA....15..193M]).

The process has been investigated thoroughly with collisionless N-Body simulations adopting high resolution models of dwarf galaxies interacting with rigid or symmetric models of hosts on orbits with high eccentricities as those of cosmological subhalos ([@2001ApJ...559..754M]; [@2001ApJ...547L.123M] ;[@2007MNRAS.378..353K]; [@2011ApJ...726...98K]). It has also been investigated in combination with ram pressure mass removal using 