Bimodal regime in young massive clusters leading to subsequent stellar
  generations
  Massive stars in young massive clusters insert tremendous amounts of mass and
energy into their surroundings in the form of stellar winds and supernova
ejecta. Mutual shock-shock collisions lead to formation of hot gas, filling the
volume of the cluster. The pressure of this gas then drives a powerful cluster
wind. However, it has been shown that if the cluster is massive and dense
enough, it can evolve in the so--called bimodal regime, in which the hot gas
inside the cluster becomes thermally unstable and forms dense clumps which are
trapped inside the cluster by its gravity. We will review works on the bimodal
regime and discuss the implications for the formation of subsequent stellar
generations. The mass accumulates inside the cluster and as soon as a high
enough column density is reached, the interior of the clumps becomes
self-shielded against the ionising radiation of stars and the clumps collapse
and form new stars. The second stellar generation will be enriched by products
of stellar evolution from the first generation, and will be concentrated near
the cluster center.
