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Table 3
Non-LTE elemental abundances of HD 48977 on the scale in which log ϵ[H] = 12.
| Element | Ion used | Lines used (Å) | HD 48977 | Nearby B stars |
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| C | C II | 5133.11 | 8.14 ± 0.10 | 8.21 ± 0.09 |
| N | N II | 3994.00, 4607.16, 4643.09, 5005.15, 5679.55 | 7.53 ± 0.12 | 7.67 ± 0.11 |
| O | O II | 4069.75, 4414.90, 4641.81, 4649.13, 4661.63, 4705.35 | 8.45 ± 0.12 | 8.51 ± 0.09 |
| Ne | Ne I | 6143.06, 6266.49, 6334.43, 6382.99, 6402.25, 6506.53 | 7.96 ± 0.12 | 7.97 ± 0.07 |
| Mg | Mg II | 7877.05 | 7.61 ± 0.10 | 7.39 ± 0.11 |
| Al | Al III | 4149.96, 4512.54, 4529.04, 5696.6, 5722.7 | 6.21 ± 0.28 | 6.13 ± 0.08 |
| Si | see Table 2 | 7.27 ± 0.20 | 7.18 ± 0.07 | |
| S | S II | 4162.48, 4524.81, 4815.55 | 7.11 ± 0.18 | 7.20 ± 0.11 |
| Fe | Fe III | 4419.60, 5156.11 | 7.21 ± 0.14 | 7.28 ± 0.10 |
Notes. Mean values obtained using the same techniques for nearby, early B-type stars showing no signs of mixing (i.e., with unaltered CNO abundances) are shown for comparison (Morel & Butler 2008; Morel et al. 2008).
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