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