Table 4
Derived abundances of HD 46769, HD 191243, and HD 184930.
| Parameter | HD 46769 | HD 191243 | HD 184930 | Solar | B stars in solar neighbourhood |
|
|
|||||
| Teff (K) | 13 000 ± 1000 | 14 000 ± 1000 | 13 000 ± 1000 | – | – |
| log g | 2.7 ± 0.1 | 2.5 ± 0.1 | 3.5 ± 0.1 | – | – |
| Si | −5.49 | −4.30 | −5.10 | −4.45 | −4.50 |
| Mg | −5.47 | −4.60 | −5.10 | −4.36 | −4.43 |
| C | −4.11 | −3.30 | −3.80 | −4.53 | −3.65 |
| N | −3.92 | −3.80 | – | −4.13 | −4.18 |
| O | – | –3.30 | – | –3.27 | –3.23 |
Notes. Metal abundances are listed as log (Nion/Ntot) and have an uncertainty of 0.2 dex. In each of the cases, n(He)/n(H) = 0.1 was kept fixed and the mass loss parameter log Q (see Kudritzki & Puls 2000 for a definition) was below −13.5. The microturbulent velocity was 10 km s-1 for HD 46769 and HD 191243, while it was 5 km s-1 for HD 184930. The solar values were taken from Asplund et al. (2009) and those of B stars in the solar neighbourhood from Simón-Díaz (2010), Nieva & Simón-Díaz (2011), and Nieva & Przybilla (2012). It was not possible to deduce an O abundance for HD 46769 and HD 184930 because their spectra do not show O ii lines, while FASTWIND does not yet have the option to predict O i lines.
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