Superbubble dynamics in globular cluster infancy II. Consequences for
  secondary star formation in the context of self-enrichment via fast rotating
  massive stars
  The self-enrichment scenario for globular clusters (GC) requires large
amounts of residual gas after the initial formation of the first stellar
generation. Recently, Krause et al. (2012) found that supernovae may not be
able to expel that gas, as required to explain their present day gas-free
state, and suggested that a sudden accretion on to the dark remnants, at a
stage when type II supernovae have ceased, may plausibly lead to fast gas
expulsion. Here, we explore the consequences of these results for the
self-enrichment scenario via fast rotating massive stars (FRMS). We analyse the
interaction of FRMS with the intra-cluster medium (ICM), in particular where,
when and how the second generation of stars may form. From the results, we
develop a timeline of the first approximately 40 Myr of GC evolution. The
results of Paper I imply three phases during which the ICM is in a
fundamentally different state, namely the wind bubble phase (lasting 3.5 to 8.8
Myr), the supernova phase (lasting 26.2 to 31.5 Myr), and the dark remnant
accretion phase (lasting 0.1 to 4 Myr): (i) Quickly after the first generation
massive stars have formed, stellar wind bubbles compress the ICM into thin
filaments. No stars may form in the normal way during this phase, due to the
high Lyman-Werner flux density. If the first generation massive stars have
however equatorial ejections, as we proposed in the FRMS scenario, accretion
may resume in the shadow of the equatorial ejecta. The second generation stars
may then form due to gravitational instability in these discs that are fed by
both the FRMS ejecta and pristine gas. [...]
