By Jean-Claude Mermilliod (auth.), Dany Vanbeveren (eds.)

A famous person in a binary may perhaps engage with its significant other and this complicates considerably its constitution and evolution. in the course of numerous many years some time past many astronomers was hoping that the variety of binaries is small. this can be occasionally mirrored in theoretical reports facing huge populations of stars the place it's ASSUMED (without any justification) that binaries don't modify the implications. The variety of proven binaries raises as observations increase and we there­ fore proposal that the time used to be correct to arrange a gathering the place the most subject could be the impact of binaries on stellar inhabitants reviews. The SOC proposed a software with prolonged normal overviews and highlights of non-evolved and advanced binaries, with low mass, intermediate mass and large elements, the hyperlink with supernova explosions, pulsars and gamma-ray bursts, the impact of binaries at the chemical evo­ lution of galaxies. experts within the diversified learn fields have been invited and feature given very fascinating and hugely academic talks. As may be spotted through examining the complaints, the authors have placed loads of attempt in getting ready their contribution.

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Reipurth & H. Zinnecker, p. -P. & Bouchet L. be Keywords: Non-evolved binaries, mass-ratio distribution, B primaries Abstract 1. Assuming that binaries originate in star forming clouds with a Salpetertype IMF an analytical expression was derived for the mass-ratio distribution for non' evolved binaries. into account in order to compare theory with observations. Theory was optimized so as to fit best with the observed q-distribution of SBls and SB2s with a non-evolved B-type primary. Many real binaries wiIl not be observed as SBls, so that the number of real SBls could be more than twice as high as observed.

However, because each technique is dedicated to specific targets, we have not been able to completely survey any open cluster and cover an domains of periods, separations and mass ratio. The Hyades is probably the only exception thanks to the systematic observing programs undertaken by Mason et al. (1993) and Patience et al. (1998) (speckle interferometry) and Stefanik & Latham (1992) (radial velocity). The example of the Pleiades mentionned in the introduction (Bouvier et al. 1997) illustrates very clearly the point.

200, Eds. B. Reipurth & H. Zinnecker, p. 49 Debernardi Y. 2000, in "Birth and Evolution of Binary Stars", poster proceedings of IAU Symp. 200, Eds. B. Reipurth & H. Zinnecker, p. 161 Duchene G. , Bouvier J. & Simon T. 1999, A&A 343,831 Duquennoy A. & Mayor M. , Mayor M. -C. 1992, in "Binaries as Tracers of Stellar Formation", Eds A. Duquennoy & M. Mayor, (Cambridge Univ. Press), p. 52 Garda B. -C. , Verbunt F. & Weinberg M. A. & Kassis M. 1997, in "Third Pacific Rim Conference on Recent Development of Binary Star Research", Ed.

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