HD 65949: Rosetta Stone or Red Herring
C. R. Cowley, S. Hubrig, P. Palmeri, P. Quinet, \'E. Bi\'emont, G. M., Wahlgren, O. Sch\"utz, and J. F. Gonz\'alez

TL;DR
This study analyzes the peculiar chemical abundance pattern of the star HD 65949, revealing complex elemental anomalies and proposing a model involving accretion and diffusion processes to explain its unusual spectrum.
Contribution
It provides detailed abundance measurements for 58 elements in HD 65949 and introduces a novel model combining accretion and diffusion to explain its unique chemical profile.
Findings
Abundance pattern resembles the N=126 r-process peak of solar material.
Significant correlation between abundance excesses and second ionization potentials.
Model predicts primary and secondary masses near 3.3 and 1.6 solar masses.
Abstract
HD 65949 is a late B star with exceptionally strong Hg II at 3984[A], but it is not a typical HgMn star. The Re II spectrum is of extraordinary strength. Abundances, or upper limits are derived here for 58 elements based on a model with Teff = 13100K, and log(g) = 4.0. Even-Z elements through nickel show minor deviations from solar abundances. Anomalies among the odd-Z elements through copper are mostly small. Beyond the iron peak, a huge scatter is found. The abundance pattern of the heaviest elements resembles the N=126 r-process peak of solar material, though not in detail. We find a significant correlation of the abundance excesses with second ionization potentials for elements with Z > 30. This indicates the relevance of photospheric or near-photospheric processes. We explore a model with mass accretion of exotic material followed by the more commonly accepted differentiation by…
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