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IR mass loss rates of LMC and SMC O stars

Published online by Cambridge University Press:  12 July 2011

Derck L. Massa ,
Alex W. Fullerton ,
Danny J. Lennon  and
Raman K. Prinja
Derck L. Massa
Affiliation:
STScI, Baltimore, MD, USA
Alex W. Fullerton
Affiliation:
STScI, Baltimore, MD, USA
Danny J. Lennon
Affiliation:
STScI, Baltimore, MD, USA
Raman K. Prinja
Affiliation:
Dept. of Astronomy, UCL, London, UK
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Abstract

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We use a combination of VJHK and Spitzer [3.6], [5.8] and [8.0] photometry, to determine IR excesses in a sample of LMC and SMC O stars. This sample is ideal for determining excesses because: 1) the distances to the stars, and hence their luminosities, are well-determined, and; 2) the very small line of sight reddenings minimize the uncertainties introduced by extinction corrections. We find IR excesses much larger than expected from Vink et al. (2001) mass loss rates. This is in contrast to previous wind line analyses for many of the LMC stars which suggest mass loss rates much less than the Vink et al. predictions. Together, these results indicate that the winds of the LMC and SMC O stars are strongly structured (clumped).

Keywords

stars: early-typestars: mass lossgalaxies: Magellanic Clouds
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S272: Active OB stars: structure, evolution, mass loss, and critical limits , July 2010 , pp. 302 - 303
Copyright
Copyright © International Astronomical Union 2011

References

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