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Recombination line abundances in the winds of the [WC] Wolf-Rayet stars

  • R. L. Kingsburgh (a1), I. Dashevsky (a1) and M. J. Barlow (a2)

Abstract

We present a preliminary abundance analysis, utilising recombination theory, for the [WC] Wolf-Rayet central stars of the planetary nebulae NGC 6751 and NGC 6905. This analysis is based on optical spectrophotometry of a sample of [WC] stars which show a strong O vi 3811, 34 å feature in emission. We have performed a recombination line analysis of stellar wind emission lines which are judged to be optically thin, in order to derive relative C, O and He abundances. We also present a comparison of the derived wind abundances with those of Population I WO stars. For the [WC 4] central star of NGC 6751, we have derived C/He = 0.35 and C/O = 4.2, by number. And for the [WC 3] central star of NGC 6905, we have derived C/He = 0.36 and C/O< 12. These surface abundances are comparable to the abundances that have been derived for early type [WC] stars via more complex NLTE modelling (e.g. Koesterke & Hamann 1996).

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References

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Howarth, I. D., 1983, MNRAS, 203, 301.
Hillier, J. D., 1989, ApJ, 347, 392.
Kingsburgh, R. L, & Barlow, M. J., 1994, MNRAS.
Kingsburgh, R. L, Barlow, M. J. & Storey, P. J., 1995, A&A, 295, 75.
Koesterke, L. & Hamann, W.-R., 1996, A&A, in press. (KH).
Smith, L. & Aller, L. H., 1969, ApJ, 157, 1245.

Recombination line abundances in the winds of the [WC] Wolf-Rayet stars

  • R. L. Kingsburgh (a1), I. Dashevsky (a1) and M. J. Barlow (a2)

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