On the sodium versus iron correlation in late B-type stars

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<jats:title>Abstract</jats:title> <jats:p>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 (10000 K ≲ Teff ≲ 14000 K) 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 in 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.</jats:p>

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