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The self-enrichment scenario for globular clusters (GC) requires largeamounts of residual gas after the initial formation of the first stellargeneration. Recently, Krause et al. (2012) found that supernovae may not beable to expel that gas, as required to explain their present day gas-freestate, and suggested that a sudden accretion on to the dark remnants, at astage when type II supernovae have ceased, may plausibly lead to fast gasexpulsion. Here, we explore the consequences of these results for theself-enrichment scenario via fast rotating massive stars (FRMS). We analyse theinteraction of FRMS with the intra-cluster medium (ICM), in particular where,when and how the second generation of stars may form. From the results, wedevelop a timeline of the first approximately 40 Myr of GC evolution. Theresults of Paper I imply three phases during which the ICM is in afundamentally different state, namely the wind bubble phase (lasting 3.5 to 8.8Myr), the supernova phase (lasting 26.2 to 31.5 Myr), and the dark remnantaccretion phase (lasting 0.1 to 4 Myr): (i) Quickly after the first generationmassive stars have formed, stellar wind bubbles compress the ICM into thinfilaments. No stars may form in the normal way during this phase, due to thehigh Lyman-Werner flux density. If the first generation massive stars havehowever equatorial ejections, as we proposed in the FRMS scenario, accretionmay resume in the shadow of the equatorial ejecta. The second generation starsmay then form due to gravitational instability in these discs that are fed byboth the FRMS ejecta and pristine gas. [...]

astronomy and astrophysics

Superbubble dynamics in globular cluster infancy II. Consequences for  secondary star formation in the context of self-enrichment via fast rotating  massive stars