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Free Access
Issue
A&A
Volume 565, May 2014
Article Number A40
Number of page(s) 14
Section Stellar structure and evolution
DOI https://doi.org/10.1051/0004-6361/201323189
Published online 01 May 2014

Online material

Table 1

Observations of SAO 244567.

thumbnail Fig. 4

Determination of Teff using the ionization equilibria of N, O, S and C in the FUSE spectrum taken in 2002. The red (thick) lines indicate the pure stellar spectrum, the blue (thin) lines also include the interstellar lines. N iiiiv, O iiiv, S ivvi and C iiiiv lines are marked.

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thumbnail Fig. 5

Same as Fig. 4, but for the year 2006.

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Table 3

Statistics of our model atoms.

thumbnail Fig. 6

Comparison of the temperature structures of a HHeCNO (blue, thin) and the final HHeCNONeSiPSFeNi model (red, thick) with Teff = 60 kK and log g = 6.0.

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thumbnail Fig. 7

Determination of the Si abundance. Synthetic line profiles calculated from models with 0.1× solar (blue, dashed), solar (green, light gray, including ISM absorption lines), and 10× solar (red, dark) Si abundance are compared with the observed Si iv (left) and Si iii (right) line profiles.

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thumbnail Fig. 8

Determination of the P abundance. Synthetic line profiles calculated from models with 0.01× solar (blue, dashed), 0.1× solar (green, light gray, including ISM absorption lines), and solar (red, dark) P abundance are compared with the observed P v line profiles.

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thumbnail Fig. 9

Determination of the Fe abundance and the upper limit for the Ni abundance. Synthetic spectra calculated from models with 0.1× solar (blue, dashed), solar (green, light) and 10× solar (red, dark) Fe and Ni abundances are compared with the observation.

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© ESO, 2014

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