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2009MNRAS.392..590B - Mon. Not. R. Astron. Soc., 392, 590-616 (2009/January-2)
Stellar, brown dwarf and multiple star properties from hydrodynamical simulations of star cluster formation.
BATE M.R.
Abstract (from CDS):
We find that hydrodynamical/sink particle simulations can reproduce many of the observed stellar properties very well. Multiplicity as a function of the primary mass, the frequency of very low mass (VLM) binaries, general trends for the separation and mass ratio distributions of binaries and the relative orbital orientations of triples systems are all in reasonable agreement with observations. We also examine the radial variations of binarity, velocity dispersion and mass function in the resulting stellar cluster and the distributions of disc truncation radii due to dynamical interactions. For VLM binaries, because their separations are typically close, we find that their frequency is sensitive to the sink particle accretion radii and gravitational softening used in the calculations. Using small accretion radii and gravitational softening results in a frequency of VLM binaries similar to that expected from observational surveys (∼20 per cent). We also find that VLM binaries evolve from wide, unequal-mass systems towards close equal-mass systems as they form. The two main deficiencies of the calculations are that they overproduce brown dwarfs relative to stars and that there are too few unequal-mass binaries with K- and G-dwarf primaries. The former of these is likely due to the absence of radiative feedback and/or magnetic fields.
Abstract Copyright: © 2008 The Author. Journal compilation © 2008 RAS
Journal keyword(s): binaries: general - stars: formation - stars: kinematics - stars: low-mass, brown dwarfs - stars: luminosity function, mass function - ISM: clouds
Errata: erratum vol. 418, p. 703 (2011)
Simbad objects: 4
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