Accretion in stellar clusters and the collisional formation of massive stars

By Ian A. Bonnell, Matthew R. Bate. 2002

161 citations recorded by the source corpus.

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In Astronomy and Astrophysics

Citations in the corpus

The Birth of High-Mass Stars: Accretion and/or Mergers? (2005, methodology): “In high density proto-clusters, interactions of single (or binary) stars with binary systems can also also lead to merging (Bonnell & Bate 2002).”
Photoionizing feedback in star cluster formation (2005, methodology): “Bonnell & Bate (2002) explored this scenario by performing numerical calculations at two resolutions.”
RADIATION-HYDRODYNAMIC SIMULATIONS OF THE FORMATION OF ORION-LIKE STAR CLUSTERS. II. THE INITIAL MASS FUNCTION FROM WINDS, TURBULENCE, AND RADIATION (2012, background): “1 M , and massive stars subsequently grow from these small seeds by Bondi-Hoyle accretion (Bonnell et al. 1997, 2001a,b, 2004, 2006; Bonnell & Bate 2002, 2006; Bate & Bonnell 2005; Smith et al. 2009a,b).”
Toward Understanding Massive Star Formation (2007, background): “It is unclear how to refute this argument, but the constant slope of the upper IMF may simply imply that stellar collisions and mergers are not a dominant factor in massive star formation, except for the most massive stars (Bonnell & Bate 2002) where statistical fluctuations can hide a slope change.”
Galactic Stellar and Substellar Initial Mass Function (2003, background): “…between the various stellar cores, and a combination of mass accretion and stellar mergers, has been proposed by Bonnel, Bate and collaborators (Bonnel et al. 2001a, 2001b, Bonnell & Bate 2002), based on hydrodynamical simulations of gas accretion onto a pre-existing cluster of 1000 stars.”
Probing the formation of intermediate- to high-mass stars in protoclusters - A detailed millimeter study of the NGC 2264 clumps (2005, background): “In the dense central region of the collapsing protocluster, the probability of encounters becomes large enough that massive stars can form by coalescence of intermediate-mass protostars (e.g. Bonnell & Bate 2002).”
Stellar, brown dwarf and multiple star properties from hydrodynamical simulations of star cluster formation (2008, background): “Earlier similar large-scale hydrodynamical calculations (Klessen, Burkert & Bate 1998; Klessen & Burkert 2000, 2001; Klessen 2001; Bonnell et al. 2001; Bonnell & Bate 2002; Bonnell, Bate & Vine 2003) formed large numbers of stars, but were unable to resolve brown dwarfs, most binaries and discs.”
On the diversity and statistical properties of protostellar discs (2018, background): “S R ] 2 3 Ja n tems and resolve discs reasonably well (e.g. to au scales), or those that study the formation of many protostars in molecular clouds but do not resolve most protostellar discs (e.g. Klessen et al. 1998; Bonnell & Bate 2002; Krumholz et al. 2012).”
Stellar, brown dwarf and multiple star properties from a radiation hydrodynamical simulation of star cluster formation (2011, methodology): “Early simulations of this type (Klessen, Burkert & Bate 1998; Klessen & Burkert 2000, 2001; Bonnell et al. 2001; Klessen 2001; Bonnell & Bate 2002; Bonnell, Bate & Vine 2003) used isothermal equations of state and produced large numbers of stars, but used sink particles (Bate, Bonnell & Price 1995)…”
Physical Processes in the Interstellar Medium (2014, background): “In the original competitive accretion picture (Bonnell et al., 2001a,b; Bonnell & Bate, 2002; Bate et al., 2003) protostars start out with roughly the same small mass close to the opacity limit of fragmentation (Rees, 1976).”
Early Evolution of Stellar Groups and Clusters: Environmental Effects on Forming Planetary Systems (2005, background): “Some previous studies (e.g., Bonnell & Bate 2002) have focused on the densest regions of large clusters where the interaction rates are high and the background environment has an important effect on star formation.”
Runaway collisions in young star clusters - II. Numerical results (2005, background): “This problem led to the proposal that the truly primordial IMF may not extend past 10M⊙ and that mergers may be —at least partially— responsible for the formation of more massive stars (Bonnell et al. 1998; Bonnell & Bate 2002; Bally & Zinnecker 2005).”
The importance of radiative feedback for the stellar initial mass function (2008, background): “Or it may be due to coalesence or collisional build-up (Silk & Takahashi 1979; Pumphrey & Scalo 1983; Bonnell, Bate & Zinnecker 1998; Bonnell & Bate 2002).”
The Initial Configuration of Young Stellar Clusters: A K-Band Number Counts Analysis of the Surface Density of Stars (2004, result): “While stellar collisions are very unlikely at the stellar densities reported in this work (cf. Bonnell & Bate 2002, and note that lower average stellar masses further increase the timescales in Figure 1 of that study), close approaches on the order of protostel- lar envelope or large T Tauri disk…”
A study of high velocity molecular outflows with an up-to-date sample (2004, background): “Among 14 high mass sources, 10 are UC HII or bright far infrared sources, which are more evolved among massive YSOs.”
Star formation through gravitational collapse and competitive accretion (2006, background): “…to overcome this obstacle, including disc accretion and radiation beaming (Yorke & Sonnhalter 2002), Rayleigh-Taylor instabilities in the accretion flow (Krumholz et al.2005b) and stellar collisions (Bonnell, Bate & Zinnecker 1998; Bonnell & Bate 2002) and binary mergers (Bonnell & Bate 2005).”
CIRCUMVENTING THE RADIATION PRESSURE BARRIER IN THE FORMATION OF MASSIVE STARS VIA DISK ACCRETION (2010, background): “Previous theoretical models focused on different points of view, namely, the competitive accretion (Bonnell et al. 1998; Bonnell & Bate 2002; Bonnell et al. 2004; Bate 2009a, 2009b) and the turbulent core model (McKee & Tan 2003), but they agree on the formation of accretion disks.”
Thermal physics, cloud geometry and the stellar initial mass function (2005, background): “The number of bound clumps formed is always comparable to the number of Jeans masses present initially, although fragment masses may be somewhat reduced by compression during the collapse (Klessen 2001; Bonnell & Bate 2002; Bate et al. 2003).”