A comprehensive set of simulations studying the influence of gas expulsion on star cluster evolution

By H. Baumgardt, Pavel Kroupa. 2007

293 citations recorded by the source corpus.

We have carried out a large set of N-body simulations studying the effect of residual-gas expulsion on the survival rate, and final properties of star clusters. We have varied the star formation efficiency (SFE), gas expulsion time-scale and strength of the external tidal field, obtaining a three-dimensional grid of models which can be used to predict the evolution of individual star clusters or whole star cluster systems by interpolating between our runs. The complete data of these simulations are made available on the internet.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/ef11a2092f589824126bc7825616bf2aa1560bbb

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In Astronomy and Astrophysics

Citations in the corpus

Young Massive Star Clusters (2010, background): “8 in Baumgardt & Kroupa 2007), where tdyn is the initial dynamical time, when the gas and the stars are still bound.”
The mass function of young star clusters in spiral galaxies (2008, background): “However, the local SFE within clusterforming clumps in GMCs has to be high to produce a bound star cluster (30%−50%; Hills 1980; Elmegreen 1983; Baumgardt & Kroupa 2007) and ultimately the mass spectrum of these clumps may be more relevant.”
Evidence for top-heavy stellar initial mass functions with increasing density and decreasing metallicity (2012, methodology): “For a star formation efficiency (SFE), ǫ = Mecl Mecl +Mgas , (1) 0.1 ǫ 0.5, rapid gas expulsion (short τM ) gives rise to a phase of strong expansion following gas expulsion and the cluster will loose stars over the tidal boundary (Baumgardt & Kroupa 2007).”
STELLAR FEEDBACK IN MOLECULAR CLOUDS AND ITS INFLUENCE ON THE MASS FUNCTION OF YOUNG STAR CLUSTERS (2009, background): “Indeed, several authors have proposed that feedback would cause a bend in the mass function of young clusters at M ∼ 105M⊙, motivated in part by the well-known turnover in the mass function of old globular clusters (Kroupa & Boily 2002; Baumgardt et al. 2008; Parmentier et al. 2008).”
The dynamical state of stellar structure in star‐forming regions (2011, background): “…largely based on the assumption of either a static gas potential1 or initial equilibrium between the stars and gas (e.g. Tutukov 1978; Adams 2000; Geyer & Burkert 2001; Boily & Kroupa 2003a,b; Baumgardt & Kroupa 2007; Parmentier et al. 2008), which need not apply to star-forming regions in nature.”
Formation and dynamical evolution of multiple stellar generations in globular clusters (2008, background): “Our N-body simulations do not include primordial gas; the effect of primordial gas expulsion would add to that of SN ejecta in triggering the cluster early expansion (see e.g. Boily & Kroupa 2003; Baumgardt & Kroupa 2007).”
On the fraction of star formation occurring in bound stellar clusters (2012, methodology): “The dashed line shows the one-to-one relation, and the dotted curve gives a parametrized γ ( ) relation that is typically found in equilibrium-type, spherically-symmetric simulations of gas expulsion (e.g. Baumgardt & Kroupa 2007).”