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Most old globular clusters (GCs) in the Galaxy are observed to have internalchemical abundance spreads in light elements. We discuss a new GC formationscenario based on hierarchical star formation within fractal molecular clouds.In the new scenario, a cluster of bound and unbound star clusters (`starcluster complex', SCC) that have a power-law cluster mass function with a slope(beta) of 2 is first formed from a massive gas clump developed in a dwarfgalaxy. Such cluster complexes and beta=2 are observed and expected fromhierarchical star formation. The most massive star cluster (`main cluster'),which is the progenitor of a GC, can accrete gas ejected from asymptotic giantbranch (AGB) stars initially in the cluster and other low-mass clusters beforethe clusters are tidally stripped or destroyed to become field stars in thedwarf. The SCC is initially embedded in a giant gas hole created by numeroussupernovae of the SCC so that cold gas outside the hole can be accreted ontothe main cluster later. New stars formed from the accreted gas have chemicalabundances that are different from those of the original SCC. Usinghydrodynamical simulations of GC formation based on this scenario, we show thatthe main cluster with the initial mass as large as [2-5]x10^5 Msun can accretemore than 10^5 Msun gas from AGB stars of the SCC. We suggest that merging ofhierarchical star cluster complexes can play key roles in stellar haloformation around GCs and self-enrichment processes of GCs.

Globular cluster formation with multiple stellar populations from hierarchical star cluster complexes