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Ion fractions and the weak wind problem

Published online by Cambridge University Press:  12 July 2011

Matthew J. Austin  and
Raman K. Prinja
Matthew J. Austin
Affiliation:
Department of Physics & Astronomy, UCL Gower Street, London WC1E 6BT, UK email: mja@star.ucl.ac.uk
Raman K. Prinja
Affiliation:
Department of Physics & Astronomy, UCL Gower Street, London WC1E 6BT, UK email: mja@star.ucl.ac.uk
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Abstract

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Some late-type O stars display anomalously weak winds, possibly due to decoupling of the main driving ions from the bulk plasma. This issue and the uncertainty about the nature of wind clumping are a challenge to line-driven wind theory and need resolving in order to fully understand hot stars. We describe the results from the computation of ion fractions for the various elements in O star winds using non-LTE code CMFGEN, including parameterisation of microclumping and X-rays.

Keywords

stars: mass lossultraviolet: stars
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. 600 - 601
Copyright
Copyright © International Astronomical Union 2011

References

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