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In the present paper, we studied by means of the SIM introduced in Del Popolo(2009), the total and DM density profiles, and the correlations among differentquantities, observed by Newman et al. (2012a,b), in seven massive and relaxedclusters, namely MS2137, A963, A383, A611, A2537, A2667, A2390. Similarly toNewman et al. (2012a,b), the total density profile, in the radius range 0.003 -0.03$r_{200}$, has a mean total density profile in agreement withdissipationless simulations. The slope of the DM profiles of all clusters isflatter than -1. The slope, $\alpha$, has a maximum value (including errors) of$\alpha=-0.88$ in the case of A2390, and minimum value $\alpha=-0.14$ forA2537. The baryonic component dominates the mass distribution at radii $< 5-10$kpc, while the outer distribution is dark matter dominated. We found ananti-correlation among the slope $\alpha$, the effective radius, $R_e$, and theBCG mass, and a correlation among the core radius $r_{core}$, and $R_e$.Moreover, the mass in 100 kpc (mainly dark matter) is correlated with the massinside 5 kpc (mainly baryons).  The behavior of the total mass density profile, the DM density profile, andthe quoted correlations can be understood in a double phase scenario. In thefirst dissipative phase the proto-BCG forms, and in the second dissipationlessphase, dynamical friction between baryonic clumps (collapsing to the center)and the DM halo flattens the inner slope of the density profile.  In simple terms, the large scatter in the inner slope from cluster tocluster, and the anti-correlation among the slope, $\alpha$ and $R_e$ is due tothe fact that in order to have a total mass density profile which is NFW-like,clusters having more massive BCGs at their centers must contain less DM intheir center. Consequently the inner profile has a flatter slope.

The flat density profiles of massive, and relaxed galaxy clusters