Accretion in stellar clusters and the initial mass function

By Ian A. Bonnell, C. Clarke, Matthew R. Bate, J. Pringle. 2001

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In Astronomy and Astrophysics

Citations in the corpus

RADIATION-HYDRODYNAMIC SIMULATIONS OF THE FORMATION OF ORION-LIKE STAR CLUSTERS. II. THE INITIAL MASS FUNCTION FROM WINDS, TURBULENCE, AND RADIATION (2012, background): “…Physics, University of California, Berkeley, Berkeley, CA 94720 Padoan & Nordlund 2002; Hennebelle & Chabrier 2008) or competitive accretion (e.g. Bonnell et al. 2001a,b), can predict a shape for the IMF, but in order to determine a characteristic scale must either appeal to additional physics…”
The First Stellar Cluster (2007, background): “The stellar mass spectrum thus depends on both the details of the initial fragmentation process (e.g. as discussed by Jappsen et al. 2005; Clark & Bonnell 2005) as well as dynamical effects in the growing cluster (Bonnell et al. 2001; Bonnell, Bate & Vine 2004).”
Theory of Star Formation (2007, background): “(2) The tidal gravitational field is negligible; when it is not, RBH is replaced by the tidal radius (Bonnell et al., 2001a).”
Intermediate - mass black holes (2003, background): “…to core collapse if the initial star formation tends to place more massive stars near the center of the cluster (for observations see Hillenbrand 1997; Hillenbrand & Hartmann 1998; Kontizas et al. 1998; Sirianni et al. 2002, and for a theoretical perspective see Larson 1982; Bonnell et al. 2001).”
Physical Processes in the Interstellar Medium (2014, background): “This could be due to the stochastic nature of gas flows in turbulent media, and/or due to N -body dynamics in dense embedded clusters (e.g. Bonnell et al., 2001a,b; Klessen, 2001a), or due to other processes that lead to stochastic protostellar mass growth.”
Star formation through gravitational collapse and competitive accretion (2006, methodology): “Unfortunately, Krumholz et al.̃(2005a) use globally averaged estimates for the gas density and the velocity instead of the local variables as used in the Bonnell et al.(2001a, 2004) numerical simulations.”
Embedded Clusters in Molecular Clouds (2003, background): “The process is highly nonlinear and, even for a cluster with initially equal mass protostellar fragments, can lead to the development of a protostellar mass spectrum similar to that of the stellar IMF (Bonnell et al. 2001b, Klessen 2001).”
The formation of a star cluster: predicting the properties of stars and brown dwarfs (2002, background): “…in molec- ular gas (e.g. Larson 1978; Motte et al. 1998; Elmegreen 2002, Padoan & Nordlund 2002), and yet others attribute it to competitive accretion of gas and dynamical interactions (e.g. Larson 1978; Zinnecker 1982; Bonnell et al. 1997, 2001a,b; Klessen et al. 1998; Klessen & Burkert 2000).”
The importance of radiative feedback for the stellar initial mass function (2008, background): “It may originate from competitive accretion of fragments (Hoyle 1953; Larson 1978; Zinnecker 1982; Bonnell et al. 1997, 2001a; Bonnell et al. 2001b; Klessen, Burkert & Bate 1998; Myers 2000).”
Toward Understanding Massive Star Formation (2007, background): “In an alternate scenario by Bonnell et al. (1997, 2001a), the compression phase is more of a transient phase due to the random motions in the selfgravitating cloud.”
The initial conditions of star formation in the Ophiuchus main cloud: Kinematics of the protocluster condensations , (2007, methodology): “Note that the small value found here for the mean condensation velocity relative to the local gas (Vmean ∼ 0.3 km s−1) is also consistent with the predictions of the competitive accretion model during the gas-dominated phase of protocluster evolution (Bonnell et al. 2001a).”
Formation and dynamical evolution of multiple stellar generations in globular clusters (2008, background): “…1997; Hillenbrand & Hartmann 1998; Fischer et al. 1998; de Grijs et al. 2002; Sirianni et al. 2002; Gouliermis et al. 2004; Stolte et al. 2006; Bonnell et al. 2001; McMillan et al. 2007) have suggested that clusters may form with a significant degree of initial mass segregation imprinted by…”
Star Formation from Galaxies to Globules (2001, background): “Another change may occur if the cluster environment is so dense that coalescence and protostar interactions affect the initial mass function (IMF; Bonnell et al. 2001).”