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2004MNRAS.351..617D - Mon. Not. R. Astron. Soc., 351, 617-629 (2004/June-3)
On the properties of young multiple stars.
DELGADO-DONATE E.J., CLARKE C.J., BATE M.R. and HODGKIN S.T.
Abstract (from CDS):
We have compared the outcome of our simulations with the properties of real stellar systems as deduced from the infrared colour-magnitude diagram of the Praesepe cluster and from spectroscopic and high-resolution imaging surveys of young clusters and the field. We find that the spread of the observed main sequence of Praesepe in the 0.4-1 M☉range appears to require that stars are indeed commonly assembled into high-order multiple systems. Similarly, observational results from Taurus and ρ Ophiuchus, or moving groups such as TW Hydrae and MBM 12, suggest that companion frequencies in young systems can indeed be as high as we predict. The comparison with observational data also illustrates two problems with the simulation results. First, low mass ratio (q < 0.2) binaries are not produced by our models, in conflict with both the Praesepe colour-magnitude diagram and independent evidence from field binary surveys. Secondly, very low-mass stars and brown dwarf binaries appear to be considerably underproduced by our simulations.
Abstract Copyright: 2004 RAS
Journal keyword(s): accretion, accretion discs - hydrodynamics - binaries: general - stars: formation
Simbad objects: 15
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