On helium-dominated stellar evolution: the mysterious role of the O(He)-type stars

Free Access

Issue		A&A Volume 566, June 2014


Article Number		A116
Number of page(s)		23
Section		Stellar atmospheres
DOI		https://doi.org/10.1051/0004-6361/201423498
Published online		25 June 2014

Online material

	Fig. 1 FUSE spectrum of K 1−27 (gray) compared with final synthetic spectra (red: pure stellar, blue: combined stellar and interstellar). The locations of photospheric lines appearing in the synthetic spectrum are marked.
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	Fig. 1 continued.
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	Fig. 2 Same as Fig. 1 for LoTr 4.
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	Fig. 2 continued.
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	Fig. 3 Same as Fig. 1 for HS 1522+6615.
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	Fig. 3 continued.
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	Fig. 4 Same as Fig. 1 for HS 2209+8229.
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	Fig. 4 continued.
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	Fig. 5 HST/COS spectrum of K 1−27 (gray) compared with final synthetic spectra (red: pure stellar, blue: combined stellar and interstellar). The locations of photospheric (red) and interstellar (blue) lines reproduced by the synthetic spectrum are marked.
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	Fig. 6 Same as Fig. 5 for LoTr 4.
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	Fig. 7 Same as Fig. 5 for HS 1522+6615.
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	Fig. 8 Same as Fig. 5 for HS 2209+8229.
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	Fig. 9 Temperature, electron density stratification, and ionization fractions of all elements in our final model of K 1−27.
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	Fig. 10 Like Fig. 9, for LoTr 4.
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	Fig. 11 Like Fig. 9, for HS 1522+6615.
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	Fig. 12 Like Fig. 9, for HS 2209+8229.
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	Fig. 21 Determination of the C abundance of HS 1522+6615. C iv lines are compared with models with different C abundances as indicated by the labels.
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	Fig. 22 Determination of the N abundance of K 1−27. N v lines in the EFOSC2 observation are compared with models with different N abundances as indicated by the labels.
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	Fig. 23 Determination of the O abundance of HS 2209+8229. O v and O vi lines are compared with models with different O abundances as indicated by the labels.
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Table 1

Statistics of the model atoms used in our TMAP calculations.

© ESO, 2014

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