2009/09/07 by M. B. N. Kouwenhoven, Kouwenhoven, M. B. N., S. P. Goodwin +11
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Astrophysics of Galaxies (astro-ph.GA) #FOS: Physical sciences #Stellar, planetary, and galactic studies #astro-ph.GA
paper · pdf · doi:10.48550/arxiv.0909.1225
4 pages, to appear in the proceedings of "BINKEY: Binaries - a Key to Comprehension of the Universe", held 8-12 June 2009 in Brno, Czech Republic
arxiv created 2009/09/07 · openalex publication_date 2009/09/07 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
Over the last decades, numerous wide (>1000 AU) binaries have been discovered in the Galactic field and halo. The origin of these wide binaries cannot be explained by star formation or by dynamical interactions in the Galactic field. We explain their existence by wide binary formation during the dissolution phase of young star clusters. In this scenario, two single stars that leave the dissolving cluster at the same time, in the same direction, and with similar velocities, form a new, very wide binary. Using N-body simulations we study how frequently this occurs, and how the orbital parameters of such binaries depend on the properties of the cluster from which they originate. The resulting wide binary fraction for individual star clusters is 1-30%, depending on the initial conditions. As most stars form as part of a binary or multiple system, we predict that a large fraction of these wide binaries are in fact wide triple and quadruple systems.