Back to the Abstract

	1 Introduction
	2 Physics of the models
	3 Basic parameters on the zero age main sequence
	4 Evolution on the main sequence
	5 Initial conditions for stars reaching nearly critical velocities
	6 Rotation of stars in clusters of various ages and metallicities
	7 Discussion of the results
	8 Possible links with the Be stars
	9 Conclusions
	References

	List of tables
	List of figures