Effects of metallicity on the instability mass ratio of low-mass contact binary systems

• Published in: Monthly notices of the Royal Astronomical Society Vol. 527; no. 1; pp. 1 - 9
• Main Authors: Wadhwa, Surjit S, Landin, Natália R, Kostić, Petar, Vince, Oliver, Arbutina, Bojan, De Horta, Ain Y, Filipović, Miroslav D, Tothill, Nicholas F H, Petrović, Jelena, Djurašević, Gojko
• Format: Journal Article
• Language: English
• Published: Oxford University Press 01.01.2024
• Subjects: stars: mass-loss; binaries: eclipsing; techniques: photometric
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1093/mnras/stad3129

ABSTRACT The orbital stability of contact binary systems has been receiving considerable attention recently. Theoretical studies indicate that merger is likely to occur at very low-mass ratios, but the actual mass ratio at which merger may take place is likely to be variable and dependent on the mass of the primary. We consider the effects of metal content on the orbital stability of contact binary systems by modelling the gyration radius of a rotating and tidally distorted primary component at various values of $\rm [Fe/H]$ in the range −1.25 to +0.5. We determine the instability mass ratio range for contact binary systems with a low-mass primary 0.6 M⊙ ≤ M1 ≤ 1.4 M⊙ at various metallicity levels and show that systems with low metallicity have an instability mass ratio lower than those with higher metal content and therefore are likely to be more stable. We illustrate the effect through light-curve analysis of two otherwise very similar contact binary systems, except for different metallicity. While both would be considered unstable if metallicity was not taken into consideration, only one remains in that category after appropriate adjustments based on metallicity have been made.