|Authors:||M. G. H. Krause 1, S. S. R. Offner 2, C. Charbonnel 3,4, and 8 co-authors|
|Affiliations:||(1) Centre for Astrophysics Research, School of Physics, Astronomy and Mathematics, University of Hertfordshire, Hertfordshire, UK; (2) Department of Astronomy, The University of Texas, Austin TX, U.S.A.; (3) Department of Astronomy, University of Geneva, Versoix, Switzerland; (4) IRAP, CNRS & Univ. of Toulouse, Toulouse, France|
|Accepted by:||Space Science Reviews, Volume 216, Issue 4, article id.64|
Star clusters form in dense, hierarchically collapsing gas clouds. Bulk kinetic energy is transformed to turbulence with stars forming from cores fed by filaments. In the most compact regions, stellar feedback is least effective in remov- ing the gas and stars may form very efficiently. These are also the regions where, in high-mass clusters, ejecta from some kind of high-mass stars are effectively cap- tured during the formation phase of some of the low mass stars and effectively channeled into the latter to form multiple populations. Star formation epochs in star clusters are generally set by gas flows that determine the abundance of gas in the cluster. We argue that there is likely only one star formation epoch after which clusters remain essentially clear of gas by cluster winds. Collisional dynamics is important in this phase leading to core collapse, expansion and eventual disper- sion of every cluster. We review recent developments in the field with a focus on theoretical work.