The Formation of Very Wide Binaries

M. B. N. Kouwenhoven; S. P. Goodwin; R. J. Parker; M. B. Davies; D. Malmberg; P. Kroupa

doi:10.48550/arXiv.0909.1225

The Formation of Very Wide Binaries

M. B. N. Kouwenhoven, S. P. Goodwin, R. J. Parker, M. B. Davies, D. Malmberg, P. Kroupa

Department of Physics

Research output: Contribution to conference › Paper › peer-review

Abstract

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.

Original language	English
DOIs	https://doi.org/10.48550/arXiv.0909.1225
Publication status	Published - 1 Dec 2010

Keywords

Astrophysics - Galaxy Astrophysics

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10.48550/arXiv.0909.1225

https://ui.adsabs.harvard.edu/abs/2010ASPC..435..165K

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title = "The Formation of Very Wide Binaries",

abstract = "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.",

keywords = "Astrophysics - Galaxy Astrophysics",

author = "Kouwenhoven, {M. B. N.} and Goodwin, {S. P.} and Parker, {R. J.} and Davies, {M. B.} and D. Malmberg and P. Kroupa",

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T1 - The Formation of Very Wide Binaries

AU - Kouwenhoven, M. B. N.

AU - Goodwin, S. P.

AU - Parker, R. J.

AU - Davies, M. B.

AU - Malmberg, D.

AU - Kroupa, P.

PY - 2010/12/1

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N2 - 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.

AB - 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.

KW - Astrophysics - Galaxy Astrophysics

U2 - 10.48550/arXiv.0909.1225

DO - 10.48550/arXiv.0909.1225

M3 - Paper

ER -

The Formation of Very Wide Binaries

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Keywords

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