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Non-LTE Spectral Analysis of PG 1159–035

  • K. Werner (a1), U. Heber (a1) and K. Hunger (a1)

Extract

We present first preliminary results from an exploratory spectral analysis of PG1159-035. An effective temperature of 120000 K (±20000 K) and a surface gravity of about log g=7 are derived from optical and ultraviolet profiles of carbon and helium lines. NLTE model atmospheres are used which are composed of H (1%), He (19%), C (40%) and O (40%, mass fractions). The abundances adopted are in accordance with predictions of stellar pulsation theory. A direct spectroscopic determination is under way. The analysis of optical CIV lines is rendered difficult due to the lack of a reliable line broadening theory which would have to account for a gradual change to broadening by linear Stark effect. Due to the complexity of the spectral analysis, reliable abundance ratios can only be derived from a systematic investigation employing a large grid of models.

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Copyright

References

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Auer, L.H., Mihalas, D.: 1969, Astrophys. J. 158, 641
Griem, H.R.: 1968, Phys. Rev. 165, 258
Husfeld, D.: 1987, IAU coll. No. 95, 237
Sahal-Bréchot, S., Segre, E.R.A.: 1971, Astron. Astrophys. 13, 161
Starrfield, S.: 1987, IAU coll. No. 95, 309
Unsöld, A.: 1968, “Physik der Sternatmosphären”, 2nd ed., Springer, Berlin
Werner, K.: 1987, in “Numerical Radiative Transfer”, ed. Kalkofen, W., Cambridge Univ.Press
Werner, K.: 1988, Astron. Astrophys. (in press)

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