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Gas expulsion or gas retention is a central issue in most of the models formultiple stellar populations and light element anti-correlations in globularclusters. The success of the residual matter expulsion or its retention withinyoung stellar clusters has also a fundamental importance in order to understandhow star formation proceeds in present-day and ancient star-forming galaxiesand if proto-globular clusters with multiple stellar populations are formed inthe present epoch. It is usually suggested that either the residual gas israpidly ejected from star-forming clouds by stellar winds and supernovaexplosions, or that the enrichment of the residual gas and the formation of thesecond stellar generation occur so rapidly, that the negative stellar feedbackis not significant. Here we continue our study of the early development of starclusters in the extreme environments and discuss the restrictions that strongradiative cooling and stellar mass segregation provide on the gas expulsionfrom dense star-forming clouds. A large range of physical initial conditions instar-forming clouds which include the star-forming cloud mass, compactness, gasmetallicity, star formation efficiency and effects of massive stars segregationare discussed. It is shown that in sufficiently massive and compact clustershot shocked winds around individual massive stars may cool before merging withtheir neighbors. This dramatically reduces the negative stellar feedback,prevents the development of the global star cluster wind and expulsion of theresidual and the processed matter into the ambient interstellar medium. Thecritical lines which separate the gas expulsion and the gas retention regimesare obtained.

Gas expulsion vs gas retention in young stellar clusters II: effects of cooling and mass segregation