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We present N-body simulations of the process of bulge formation in discgalaxies due to inward migration of massive stellar clumps. The process isaccompanied by dark halo heating, with a quasi-isothermal core replacing theinitial central density cusp, transforming an initially dark matter dominatedcentral region into a baryon dominated one. The characteristics of the clumpsare chosen to be compatible with low redshift observations of stellar clumps inDYNAMO-HST galaxies, which may be relatively long lived in terms of beingrobust against internal starburst-instigated disruption. We thus test fordisruption due to tidal stripping using different clump internal radialprofiles; Plummer, Hernquist and Jaffe, in ascending order of steeper centraldensity profile. Our calculations predict that in order for clump migration tobe effective in building galactic bulges and dark halo cores, steeplyincreasing central clump profiles, or a less massive or less concentratedhaloes, are preferred. The dependence on such factors may contribute to thediversity in observed total mass distributions and resulting rotation curves ingalaxies. When the process is most efficient, a 'bulge-halo conspiracy', with asingular isothermal total density akin to that observed bright galaxies,results.

Building stellar bulges and halo cores from massive clumps observed in the DYNAMO-HST sample