Multivariate Statistical Analysis of Low Mass Ratio Contact Binaries: Definition, Dynamical Stability, and Parameter Relationships

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Original abstract

This study explores multiple aspects of W Ursae Majoris (W UMa) contact binary systems with low mass ratios, providing empirical insights into their definition, structure, rotational stability, and parameter relationships. We first examined the range of mass ratios that characterize these systems and, based on an analysis of 818 contact binaries, established an empirical threshold of $q \approx 0.27$ to identify low mass ratio systems. To investigate rotational stability, we conducted a Monte Carlo analysis of the squared gyration radii ($k_1^2$ and $k_2^2$) and assessed the resulting spin-to-orbital angular momentum ratio ($J_\mathrm{spin}/J_\mathrm{orb}$), finding that while $k_1$ remains nearly constant, $k_2$ and $J_\mathrm{spin}/J_\mathrm{orb}$ decrease slightly with increasing mass ratio, emphasizing the role of the secondary star's internal structure. Moreover, we compiled a dedicated sample of 115 low mass ratio contact binaries and estimated their absolute parameters using Gaia DR3 parallaxes. From this dataset, we derived empirical parameter relationships for low mass ratio systems, which provide a useful reference for future observational and theoretical studies. The resulting datasets and statistical summaries offer benchmarks for modeling, stability evaluation, and evolutionary studies of W UMa-type binaries with low mass ratios.

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