Effects of Metallicity on the Instability Mass Ratio of Low Mass Contact Binary Systems

TL;DR

This study investigates how metallicity influences the orbital stability of low-mass contact binary systems, revealing that lower metallicity systems tend to be more stable and providing a method to assess stability considering metallicity effects.

Contribution

It introduces a model for the impact of metallicity on the instability mass ratio in contact binary systems, highlighting the importance of metallicity in stability analysis.

Findings

Lower metallicity systems have lower instability mass ratios.

Metallicity significantly affects the stability thresholds of contact binaries.

Light curve analysis confirms metallicity's role in stability assessment.

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 metallicity in the range -1.25 to +0.5. We determine the instability mass ratio range for contact binary systems with a low mass primary in the range 0.6M(sun) to 1.4M(sun) 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.