The initial period function of late-type binary stars and its variation

TL;DR

This study investigates the initial period distribution of late-type binary stars, suggesting a potentially universal initial period function that evolves through disruption in star clusters, aligning pre-main sequence and main sequence observations.

Contribution

It proposes a universal initial period function for late-type binaries, supported by analysis of multiple star-forming regions and consistency with dynamical population synthesis models.

Findings

Pre-main sequence populations differ from main sequence in period distribution.

A universal initial period function can explain observed variations after disruption.

The initial period function may be flat in log-P or log-semi-major axis.

Abstract

The variation of the period distribution function of late-type binaries is studied. It is shown that the Taurus--Auriga pre-main sequence population and the main sequence G dwarf sample do not stem from the same parent period distribution with better than 95 per cent confidence probability. The Lupus, Upper Scorpius A and Taurus--Auriga populations are shown to be compatible with being drawn from the same initial period function (IPF), which is inconsistent with the main sequence data. Two possible IPF forms are used to find parent distributions to various permutations of the available data which include Upper Scorpius B (UScB), Chameleon and Orion Nebula Cluster pre-main sequence samples. All the pre-main sequence samples studied here are consistent with the hypothesis that there exists a universal IPF which is modified through binary-star disruption if it forms in an embedded star cluster leading to a general decline of the observed period function with increasing period. The pre-main sequence data admit a log-normal IPF similar to that arrived at by Duquennoy & Mayor (1991) for main sequence stars, provided the binary fraction among pre-main sequence stars is significantly higher. But, for consistency with proto-stellar data, the possibly universal IPF ought to be flat in log-P or log-semi-major axis and must be similar to the K1 IPF form derived through inverse dynamical population synthesis, which has been shown to lead to the main sequence period function if most stars form in typical embedded clusters.