Abstract
From high-resolution spectra a non-local thermodynamic equilibrium analysis of the Mg II 4481.2-A feature is implemented for 52 early and medium local B stars on the main sequence (MS). The influence of the neighbouring line Al III 4479.9-A is considered. The magnesium abundance is determined; it is found that log e(Mg) = 7.67 ± 0.21 on average. It is shown that uncertainties in the microturbulent parameter V t are the main source of errors in log e(Mg). When using 36 stars with the most reliable V t values derived from On II and N II lines, we obtain the mean abundance log e(Mg) = 7.59 ± 0.15. The latter value is precisely confirmed for several hot B stars from an analysis of the Mg II 7877-A weak line. The derived abundance log e(Mg) = 7.59 ± 0.15 is in excellent agreement with the solar magnesium abundance log e ○. (Mg) = 7.55 ± 0.02, as well as with the proto-Sun abundance log e ps (Mg) = 7.62 ± 0.02. Thus, it is confirmed that the Sun and the B-type MS stars in our neighbourhood have the same metallicity.
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