Visual Binary Separations as Functions of Primary Types, Ages, and Locations

Summary

We studied samples from the Bright Star Catalogue of B1–B7, F3–G2, and KM dwarfs for frequencies of visual companions and their separations. The frequency of detected companions does not vary significantly along the Main Sequence. But the most frequent separations and the limiting separations vary markedly along the main sequence: the limiting separations are 42000 AU for the B stars to 800 AU for the M dwarfs. This confirms results found by Öpik in 1924. Stars off the Main Sequence (giants, white dwarfs) show consistent results, as do members of Trapezium systems, hierarchical multiple-star systems, the widest known cataloged binaries, and binaries in a moving cluster (Ursa Major Stream).

We propose a scenario in which binaries in open clusters can have large separations, but after they leave the cluster environments, chance encounters with field stars and molecular clouds will disrupt all but the more compact systems. The comoving pairs discussed by Luyten, Eggen, and others are seen as members of disrupting clusters and still retaining the common cluster motions. However, the velocity dispersions within clusters ensure that the comoving pairs have similar, but not identical, motions, whereas members of truly bound binaries would have motions that are indistinguishable. Appropriate measurements should distinguish between wide binaries and the comoving pairs, which can have separations up to the outer diameters or more of open clusters.