Table 2: Mass limits for the different evolutionary scenarios (see text).
Z $\upsilon _{\rm ini}$ M $_{\rm WR}$ M $_{\rm OWR}$

[km s^-1] [ $M_{\odot }$ ] [ $M_{\odot }$ ]

0.040 0 29 42

0.040 300 21 39

0.020 0 37 62

0.020 300 22 45

0.008 300 25 69

0.004 300 32 75

**Table 2:** Mass limits for the different evolutionary scenarios (see text).
Z	$\upsilon _{\rm ini}$	M $_{\rm WR}$	M $_{\rm OWR}$
	[km s^-1]	[ $M_{\odot }$ ]	[ $M_{\odot }$ ]
0.040	0	29	42
0.040	300	21	39
0.020	0	37	62
0.020	300	22	45
0.008	300	25	69
0.004	300	32	75

Source LaTeX | All tables | In the text

	1 Introduction
	2 Physics of the models
	3 Evolution of the rotational velocities at various metallicities
	4 Evolutionary tracks, lifetimes and final masses
	5 Rotating models of Wolf-Rayet stars
	6 Comparison with the observed properties of Wolf-Rayet star populations
	7 Evolution of the surface abundances
	8 Conclusion
	References