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Dusty LBV Nebulae: Tracing the Mass Loss History of the Most Massive Stars

Published online by Cambridge University Press:  12 April 2016

Laurens B.F.M. Waters ,
Robert H.M. Voors ,
Patrick W. Morris ,
Norman R. Trams ,
Alex de Koter  and
Henny J.G.L.M. Lamers
Laurens B.F.M. Waters
Affiliation:
Astronomical Institute ‘Anton Pannekoek’, University of Amsterdam, Kruislaan 403, NL-1098 SJ Amsterdam, The Netherlands SRON Laboratory for Space Research Groningen, P.O. Box 800, NL-9700 AV Grogingen, the Netherlands
Robert H.M. Voors
Affiliation:
SRON Laboratory for Space Research Utrecht, Sorbonnelaan 2, NL-3584 CA Utrecht, the Netherlands
Patrick W. Morris
Affiliation:
Astronomical Institute ‘Anton Pannekoek’, University of Amsterdam, Kruislaan 403, NL-1098 SJ Amsterdam, The Netherlands SRON Laboratory for Space Research Utrecht, Sorbonnelaan 2, NL-3584 CA Utrecht, the Netherlands
Norman R. Trams
Affiliation:
Astrophysics Division, ESA Space Science Department, ESTEC, Keplerlaan 1, Noordwijk, The Netherlands
Alex de Koter
Affiliation:
Astronomical Institute ‘Anton Pannekoek’, University of Amsterdam, Kruislaan 403, NL-1098 SJ Amsterdam, The Netherlands
Henny J.G.L.M. Lamers
Affiliation:
SRON Laboratory for Space Research Utrecht, Sorbonnelaan 2, NL-3584 CA Utrecht, the Netherlands

Abstract

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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.

Type
Session VI Evolutionary Aspects
Information
International Astronomical Union Colloquium , Volume 169: Variable and Non-spherical Stellar Winds in Luminous Hot Stars , 1999 , pp. 381 - 390
Copyright
Copyright © Springer-Verlag 1999

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