Table 2.
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Diagnostic spectral lines for WN stars (Smith et al. 1996) and for WC stars (Crowther et al. 1998). The line strengths are measured by the peak-to-continuum ratios rather than the equivalent widths of the lines.

classElement – ionization stage – wavelength [Å]
WNa:He i λ 5875He ii λ 5411C iv λ 5808N iii λ 4640N iv λ 4057N v λ 4604
WC:He i λ 5875He ii λ 4686C ii λ 4267C iii λ 5696C iv λ 5808O v λ 5590O vi λ 3818
classElement – ionization stage – wavelength [Å]
WNa:He i λ 5875He ii λ 5411C iv λ 5808N iii λ 4640N iv λ 4057N v λ 4604
WC:He i λ 5875He ii λ 4686C ii λ 4267C iii λ 5696C iv λ 5808O v λ 5590O vi λ 3818

aThe same diagnostic lines were used for the WNh-star models.

Table 2.
Open in new tab

Diagnostic spectral lines for WN stars (Smith et al. 1996) and for WC stars (Crowther et al. 1998). The line strengths are measured by the peak-to-continuum ratios rather than the equivalent widths of the lines.

classElement – ionization stage – wavelength [Å]
WNa:He i λ 5875He ii λ 5411C iv λ 5808N iii λ 4640N iv λ 4057N v λ 4604
WC:He i λ 5875He ii λ 4686C ii λ 4267C iii λ 5696C iv λ 5808O v λ 5590O vi λ 3818
classElement – ionization stage – wavelength [Å]
WNa:He i λ 5875He ii λ 5411C iv λ 5808N iii λ 4640N iv λ 4057N v λ 4604
WC:He i λ 5875He ii λ 4686C ii λ 4267C iii λ 5696C iv λ 5808O v λ 5590O vi λ 3818

aThe same diagnostic lines were used for the WNh-star models.

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