The binarity of Milky Way F,G,K stars as a function of effective temperature and metallicity

TL;DR

This study estimates the fraction of F,G,K stars with close binary companions using multi-epoch spectra, revealing a dependence on stellar temperature and metallicity, with metal-rich stars less likely to have close binaries.

Contribution

It introduces a Bayesian method to infer close binary fractions from spectral data, highlighting the impact of metallicity on binary star occurrence.

Findings

Overall close binary fraction is approximately 43% in SDSS and 30% in LAMOST samples.

Close binary fraction decreases with increasing stellar effective temperature.

Metal-rich stars are significantly less likely to have close binary companions.

Abstract

We estimate the fraction of F,G,K stars with close binary companions by analysing multi-epoch stellar spectra from SDSS and LAMOST for radial velocity (RV) variations. We employ a Bayesian method to infer the maximum likelihood of the fraction of binary stars with orbital periods of 1000 days or shorter, assuming a simple model distribution for a binary population with circular orbits. The overall inferred fraction of stars with such a close binary companion is 43.0% \pm 2.0% for a sample of F, G, K stars from SDSS SEGUE, and 30% \pm 8.0% in a similar sample from LAMOST. The apparent close binary fraction decreases with the stellar effective temperature. We divide the SEGUE and LEGUE data into three subsamples with different metallicity ([Fe/H] < -1.1; -1.1 < [Fe/H] < -0.6; -0.6 < [Fe/H]), for which the inferred close binary fractions are 56% \pm 5.0%, 56.0% \pm 3%, and 30% \pm 5.7%. The metal-rich stars from our sample are therefore substantially less likely to possess a close binary companion than otherwise similar stars drawn from metal-poor populations. The different ages and formation environments of the Milky Way's thin disk, thick disk and halo may contribute to explaining these observations. Alternatively metallicity may have a significant effect on the formation and/or evolution of binary stars.