Journal
PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES
Volume 368, Issue 1913, Pages 733-754Publisher
ROYAL SOC
DOI: 10.1098/rsta.2009.0262
Keywords
hydrodynamics; stars: formation; stars: mass function; open clusters and associations: general
Categories
Funding
- STFC [ST/G00269X/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/H00243X/1, ST/G00269X/1] Funding Source: researchfish
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We review progress in numerical simulations of star cluster formation. These simulations involve the bottom-up assembly of clusters through hierarchical mergers, which produces a fractal stellar distribution at young (approx. 0.5 Myr) ages. The resulting clusters are predicted to be mildly aspherical and highly mass-segregated, except in the immediate aftermath of mergers. The upper initial mass function within individual clusters is generally somewhat flatter than for the aggregate population. Recent work has begun to clarify the factors that control the mean stellar mass in a star-forming cloud and also the efficiency of star formation. The former is sensitive to the thermal properties of the gas while the latter depends both on the magnetic field and the initial degree of gravitational boundedness of the natal cloud. Unmagnetized clouds that are initially bound undergo rapid collapse, which is difficult to reverse by ionization feedback or stellar winds.
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