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Article Contents
1 Introduction
2 Theoretical context
3 Method to calculate $\vec{\dot{M}}$
4 The assumptions of the model grid
5 The predicted mass-loss rates and bi-stability jumps
6 The relative importance of Fe and CNO elements in the line acceleration at low $\vec Z$
7 The global metallicity dependence
8 Complete mass-loss recipe
9 Comparison between theoretical $\vec{\dot{M}}$ and observations at subsolar $\vec Z$
10 Summary and conclusions
References

Copyright ESO 2001
Published by EDP Sciences