Scenario II: Distance (top panel) and relative velocity (bottom panel) between the centre of mass of the dark matter component and the younger stellar component for different models as a function of time: Model M8 (A1M1) with the Burkert dwarf model D1, model M9 (A1M6), with the more massive Burkert D2, model M11 (SZM4) with the compact massive dwarf model D3, and models M13 (S7M3) and M14 (S7M4) with the NFW dark halos dwarf model D4. The red line corresponds to the offset between the old and younger stellar components in Leo T (35 pc), and the blue line to the 80 pc HI-stellar offset. The gray vertical line marks the lower age limit of the younger stellar component (de Jong et al. 2008). The simulations show that the younger stellar component decays faster in the models with a compact cored M11 (SZM4) and cuspy M13 (S7M3 with radial offset), M14 (S7M4, with circular orbit offset) dark halos, than in the models with large dark matter cores M8(A1M1) and M9(A1M6).