2017MNRAS.468.3461T

Wide gravitationally bound pairs of stars can be formed from adjacent pre-stellar cores that happen to move slowly enough relative to each other. These binaries are remnants of primordial clustering. It is shown that the expected fraction of wide bound pairs in low-density star formation regions can be larger than the fraction of wide pairs in the field. However, wide binaries do not form or survive in dense clusters. Recent works on the separation distribution of young binaries, summarized here, confirm these expectations. Alternative formation mechanisms of wide binaries, such as cluster dissolution or unfolding of triple stars, cannot explain the large observed fraction of young wide pairs, and therefore are not dominant. The fact that more than half of the wide pairs contain subsystems matches the general multiplicity statistics and does not imply that hierarchical multiplicity and wide binaries are genetically related.