On the Sodium versus Iron Correlation in Late B-Type Stars

With an aim to study whether the close correlation between [Na/H] and [Fe/H] recently found in A-type stars further persists in the regime of B-type stars, the abundances of Na were determined for 30 selected sharp-lined late B-type stars (10000K < T_eff < 14000K) from the Na I 5890/5896 doublet. These Na abundances were then compared with the O and Fe abundances (derived from the O I 6156-8 and Fe II 6147/6149 lines) showing anti-correlated peculiarities. It turned out that, unlike the case of A-type stars, [Na/H] is roughly constant at a slightly subsolar level ([Na/H] ~ -0.2 (+/-0.2)) without any significant correlation with [Fe/H] which shows considerable dispersion ranging from ~ -0.6 to ~ +1.0. This may serve as an important observational constraint for understanding the abundance peculiarities along with the physical mechanism of atomic diffusion in upper main-sequence stars of late A through late B-type including Am and HgMn stars.

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