and distribution of VL2 satellites. The differences between our model and Z12 or B13 have been reported in the introduction.

In summary the method is based on the following ideas and is divided into two main phases:

1.  In the first phase, the satellite is considered isolated, without interactions with the host halo, and the flattening of the density profile produced by baryonic physics is calculated (in particular, the lowering of the central mass of subhaloes) in the same fashion as in, e.g., Del Popolo [*et al.*]{} (2014) (see also Hiotelis & Del Popolo 2006, 2013, to have a semi-analytical description of halos growth.). In this paper we deliberately chose not to take account of SF and to concentrate on the model of baryonic clumps exchanging energy and angular momentum with DM through DF, since it has clearly been shown (Del Popolo, 2014c, Fig. 4) that in the mass (circular velocity) range of the dwarfs studied in the present paper, the former is less efficient in transforming cusps into cores than the latter. Del Popolo & Hiotelis (2014) compared also the result of the current model, adding SF, to the SPH simulations of Inoue & Saitoh (2012): the full model 