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The HI Brα and Pfγ Lines Formed in the Wind from S106IR

  • J. C. Bunn
  • J. E. Drew
Conference paper
Part of the Astrophysics and Space Science Library book series (ASSL, volume 186)

Abstract

Garden and Geballe (1986) obtained high resolution, high S/N observations of the HI Brα and Pfγ lines formed in the wind from the high mass YSO S 106IR. These lines show interesting features: within the errors the red wings of the lines match but Pfγ is asymmetric with an excess of flux in the blue wing making it wider than Brα. We have developed spherically-symmetric LTE models to try to reproduce these line profiles and fluxes. These models integrate the equation of transfer through the stellar wind and include opacities due to free-free and bound-free processes as well as that due to the line itself. We find these continuum opacities can have a significant effect on the line profiles when NLTE effects are taken into account.

Keywords

Line Profile Stellar Wind Blue Wing Continuum Opacity NLTE Model 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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References

  1. Bunn, J.C., Drew, J.E.: 1991, On the origin of the HI line emission associated with massive young stellar objects, submitted to M.N.R.A.S.Google Scholar
  2. Drew, J.E.: 1990, in Properties of Hot Luminous Stars, ed. C.D. Garmany, Astronomical Society of the Pacific Conference Series, 7, 230Google Scholar
  3. Felli, M., Staude, H.J., Reddmann, T., Massi, M., Eiroa, C., Hefele, H., Neckel, T., Panagia, N.: 1984, Astron. Astrophys. 135, 261ADSGoogle Scholar
  4. Garden, R.P., Geballe, T.R.: 1986, M.N.R.A.S. 220, 611ADSGoogle Scholar
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  6. Simon, M., Felli, M., Cassar, L., Fischer, J., Massi, M.: 1983, Astrophys. J. 266 623ADSCrossRefGoogle Scholar

Copyright information

© Springer Science+Business Media Dordrecht 1993

Authors and Affiliations

  • J. C. Bunn
    • 1
  • J. E. Drew
    • 1
  1. 1.Department of PhysicsOxford UniversityUK

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