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Over the last decades, numerous wide (>1000 AU) binaries have been discoveredin the Galactic field and halo. The origin of these wide binaries cannot beexplained by star formation or by dynamical interactions in the Galactic field.We explain their existence by wide binary formation during the dissolutionphase of young star clusters. In this scenario, two single stars that leave thedissolving cluster at the same time, in the same direction, and with similarvelocities, form a new, very wide binary. Using N-body simulations we study howfrequently this occurs, and how the orbital parameters of such binaries dependon the properties of the cluster from which they originate. The resulting widebinary fraction for individual star clusters is 1-30%, depending on the initialconditions. As most stars form as part of a binary or multiple system, wepredict that a large fraction of these wide binaries are in fact wide tripleand quadruple systems.

The formation of very wide binaries