Abstract
Abstract The identification of binary stars of different mass ratios in resolved stellar populations is a challenging task. We show how the photometric diagram constructed with the pseudocolors (H-W2)-W1 versus W2-(BP-K) can be employed to estimate the binary and multiple star ratios and the distribution of their component mass ratio q effectively. As an application, we investigate the Pleiades star cluster in the range of primary component mass between 0.5 and 1.8 M ⊙. The binary star ratio is found to be between 0.54 ± 0.11 and 0.70 ± 0.14. On the other hand, the ratio of systems with a multiplicity of more than two is between 0.10 ± 0.00 and 0.14 ± 0.01. The distribution of the component mass ratio q has been approximated by a power law with the exponent between −0.53 ± 0.10 and −0.63 ± 0.22. Below 0.5 M ⊙, we expect a large number of brown dwarfs among secondary components.
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
