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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