This work is part of a long-term observational campaign conducted at the Catania Astrophysical Observatory to investigate the chemical and dynamical properties of Ap and Am stars. This study continues a series of precursor papers aimed at enhancing our understanding of peculiar stars in binary systems. We aim to provide a comprehensive characterization of ten new double-lined spectroscopic binary systems suspected of containing components with chemical peculiarities. The primary objectives are to confirm these anomalies through detailed abundance analysis, derive precise orbital elements, and determine the physical parameters of both stellar components. We acquired time-series high-resolution spectroscopy over ten years using the Catania Astrophysical Observatory Spectropolarimeter (CAOS). Radial velocities were measured via cross-correlation and modeled to obtain orbital solutions. Atmospheric parameters (T_ eff, łog g) were determined through composite Balmer line fitting, and chemical abundances for 20 elements were derived using spectral synthesis with ATLAS9 models and SYNTHE codes. In eight out of the ten investigated systems, at least one component exhibits Am-type chemical peculiarities. The targets are all in the hydrogen-burning phase, with ages of sim63 Myr -- 1 Gyr and masses of sim1 -- 4 M_⊙. For the He-weak Bp star HD, 161480, we detected a phase shift of Δϕ ≈ 1. 44 rad between the He I triplet and singlet lines, evidence of vertical chemical stratification in its atmosphere. This study successfully broadens the statistical sample of peculiar stars in binary systems. The results emphasize the complex interplay between atomic diffusion and binary dynamics, particularly through the discovery of vertical stratification in HD 161480, which highlights the need for depth-dependent atmospheric modeling in chemically peculiar stars.
Catanzaro et al. (Sun,) studied this question.
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