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We propose that there is an evolutionary link between ultra-compact bluedwarf galaxies (UCBDs) with active star formation and nucleated dwarfs based onthe results of numerical simulations of dwarf-dwarf merging. We consider theobservational fact that low-mass dwarfs can be very gas-rich, and therebyinvestigate the dynamical and chemical evolution of very gas-rich, dissipativedwarf-dwarf mergers. We find that the remnants of dwarf-dwarf mergers can bedominated by new stellar populations formed from the triggered starbursts andconsequently can have blue colors and higher metallicities (Z~[0.2-1]Z_sun). Wealso find that the remnants of these mergers can have rather highmass-densities (10^4 M_sun pc^-3) within the central 10 pc and small half-lightradii (40-100 pc). The radial stellar structures of some merger remnants aresimilar to those of nucleated dwarfs. Star formation can continue in nucleargas disks (R<100 pc) surrounding stellar galactic nuclei (SGNs) so that theSGNs can finally have multiple stellar populations with different ages andmetallicities. These very compact blue remnants can be identified as UCBDs soonafter merging and as nucleated dwarfs after fading of young stars. We discussthese results in the context of the origins of metal-rich ultra-compact dwarfs(UCDs) and SGNs.

Formation of ultra-compact blue dwarf galaxies and their evolution into nucleated dwarfs