Skip to main content Accessibility help
×
Home

The hydrogen/helium ratio on the surface of Wolf-Rayet stars

  • Peter S. Conti (a1) and Philip Massey (a1)

Extract

As yet there have been few detailed analyses of Wolf-Rayet (WR) emission line spectra. Such analyses must certainly take account of line transfer in a spherically extended, expanding medium, a problem not yet completely addressed in the complexity of WR envelopes. However, visual examination of optical spectra suggests real differences in line strengths among the Balmer and Pickering series lines in WN stars. If hydrogen is present, the Balmer lines will be stronger than the adjacent Pickering lines of ionized helium; if hydrogen is weak or absent, then there will be a smooth transition in intensities along the Pickering series with no additional contribution from the Balmer lines at alternatively blending wavelengths (Underhill 1967).

    • Send article to Kindle

      To send this article to your Kindle, first ensure no-reply@cambridge.org is added to your Approved Personal Document E-mail List under your Personal Document Settings on the Manage Your Content and Devices page of your Amazon account. Then enter the ‘name’ part of your Kindle email address below. Find out more about sending to your Kindle. Find out more about sending to your Kindle.

      Note you can select to send to either the @free.kindle.com or @kindle.com variations. ‘@free.kindle.com’ emails are free but can only be sent to your device when it is connected to wi-fi. ‘@kindle.com’ emails can be delivered even when you are not connected to wi-fi, but note that service fees apply.

      Find out more about the Kindle Personal Document Service.

      The hydrogen/helium ratio on the surface of Wolf-Rayet stars
      Available formats
      ×

      Send article to Dropbox

      To send this article to your Dropbox account, please select one or more formats and confirm that you agree to abide by our usage policies. If this is the first time you use this feature, you will be asked to authorise Cambridge Core to connect with your <service> account. Find out more about sending content to Dropbox.

      The hydrogen/helium ratio on the surface of Wolf-Rayet stars
      Available formats
      ×

      Send article to Google Drive

      To send this article to your Google Drive account, please select one or more formats and confirm that you agree to abide by our usage policies. If this is the first time you use this feature, you will be asked to authorise Cambridge Core to connect with your <service> account. Find out more about sending content to Google Drive.

      The hydrogen/helium ratio on the surface of Wolf-Rayet stars
      Available formats
      ×

Copyright

References

Hide All
Conti, P.S.: 1976, Mem. Soc. R. Sci. Liege, Ser 6, 9, p. 193.
Smith, L.F.: 1973, in “Wolf-Rayet and High Temperature Stars,IAU Symp. No. 49, eds. Bappu, V. K. and Sahade, J. (Dordrecht: Reidel).
Underhill, A.B.: 1967, Bull. Astron. Instit. Neth. 19, 173.
Underhill, A.B.: 1973, in “Wolf-Rayet and High Temperature Stars,IAU Symp. No. 49, eds. Bappu, V. K. and Sahade, J.(Dordrecht: Reidel).

The hydrogen/helium ratio on the surface of Wolf-Rayet stars

  • Peter S. Conti (a1) and Philip Massey (a1)

Metrics

Full text views

Total number of HTML views: 0
Total number of PDF views: 0 *
Loading metrics...

Abstract views

Total abstract views: 0 *
Loading metrics...

* Views captured on Cambridge Core between <date>. This data will be updated every 24 hours.

Usage data cannot currently be displayed