Dusty LBV nebulae: Tracing the mass loss history of the most massive stars

  • Laurens B. F. M. Waters
  • Robert H. M. Voors
  • Patrick W. Morris
  • Norman R. Trams
  • Alex de Koter
  • Henny J. G. L. Lamers
Evolutionary Aspects
First Online:
Part of the Lecture Notes in Physics book series (LNP, volume 523)

Abstract

We present spectra obtained with the Infared Space Observatory (ISO) of the dust shells surrounding several Luminous Blue Variables (LBVs), both in our galaxy and in the LMC. The 20–45 µm spectra of R71, AG Car and Wra 751 show prominent emission features from crystalline silicates. The composition of the crystalline silicates in LBV dust shells is compared to that found in other types of objects, such as (post)-AGB stars and red supergiants (RSG). Both Wra 751 and AG Car have a high ratio of pyroxenes to olivines. This suggests that the grains in both stars experienced very similar processing, but that this processing has lead to a higher abundance of pyroxenes compared to RSG. The dust composition of the three LBVs discussed here suggests dust formation in a cool outflow not unlike those of RSG.

Keywords

Massive Star Mass Loss Rate Dust Shell Crystalline Silicate Band Strength 
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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Copyright information

© Springer-Verlag 1999

Authors and Affiliations

  • Laurens B. F. M. Waters
    • 1
    • 2
  • Robert H. M. Voors
    • 3
  • Patrick W. Morris
    • 3
    • 1
  • Norman R. Trams
    • 4
  • Alex de Koter
    • 1
  • Henny J. G. L. Lamers
    • 3
  1. 1.Astronomical Institute ’Anton Pannekoek’University of AmsterdamAmsterdamThe Netherlands
  2. 2.SRON Laboratory for Space Research GroningenGrogingenthe Netherlands
  3. 3.SRON Laboratory for Space Research UtrechtUtrechtthe Netherlands
  4. 4.Astrophysics Division, ESA Space Science DepartmentESTECNoordwijkThe Netherlands

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