The Physics of Star Cluster Formation and Evolution
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The Physics of Star Cluster Formation and Evolution Martin G.H. Krause1 · Stella S.R. Offner2 · Corinne Charbonnel3,4 · Mark Gieles5,6 · Ralf S. Klessen7 · Enrique Vázquez-Semadeni8 · Javier Ballesteros-Paredes8 · Philipp Girichidis9 · J.M. Diederik Kruijssen10 · Jacob L. Ward10 · Hans Zinnecker11
Received: 31 January 2020 / Accepted: 11 May 2020 © Springer Nature B.V. 2020
Abstract 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 removing 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 captured during the formation phase of some of the low mass stars and 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 Star Formation Edited by Andrei Bykov, Corinne Charbonnel, Patrick Hennebelle, Alexandre Marcowith, Georges Meynet, Maurizio Falanga and Rudolf von Steiger
B M.G.H. Krause
[email protected]
1
Centre for Astrophysics Research, School of Physics, Astronomy and Mathematics, University of Hertfordshire, College Lane, Hatfield, Hertfordshire AL10 9AB, UK
2
Department of Astronomy, The University of Texas, Austin TX, 78712, USA
3
Department of Astronomy, University of Geneva, Chemin de Pegase 51, 1290 Versoix, Switzerland
4
IRAP, CNRS & Univ. of Toulouse, 14, av. E. Belin, 31400 Toulouse, France
5
Institut de Ciències del Cosmos (ICCUB-IEEC), Universitat de Barcelona, Martí i Franquès 1, 08028 Barcelona, Spain
6
ICREA, Pg. Lluis Companys 23, 08010 Barcelona, Spain
7
Zentrum für Astronomie, Institut für Theoretische Astrophysik, Universität Heidelberg, Albert-Ueberle-Str. 2, 69120 Heidelberg, Germany
8
Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de Méxíco, Campus Morelia, Apdo. Postal 3-72, Morelia 58089, México
9
Leibniz-Institut für Astrophysik (AIP), An der Sternwarte 16, 14482 Potsdam, Germany
10
Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstraße 12-14, 69120 Heidelberg, Germany
11
Nucleo de Astroquimica y Astrofisica, Universidad Autonoma de Chile, Avda Pedro de Valdivia 425, Providencia, Santiago de Chile, Chile
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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 dispersion of every cluster. We review recent developments in the field with a focus on theoretical work. Keywords Galaxies: star clusters: general · ISM: kinematics and dynamics · Open clusters and associations: general · Stars: formation
1 Star Clusters: More than a Collection of Stars Star clusters have caught human a
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