Table 4: Comparison of resulting WR masses and orbital periods from non-rotating and rotating binary systems with the same initial parameters. $M_{\rm 1,in},M_{\rm 2,in}$ are initial primary and secondary mass, $p_{\rm in}$ is the initial orbital period, $M_{\rm WR,5}$ , $M_{\rm WR,1}$ are WR masses at $X_{\rm s}=0.05$ and $X_{\rm s}\le 0.01$ respectively and p is the orbital period in the initial WR+O system where the hydrogen surface abundance of WR star is $X_{\rm s}=0.05$ . Systems are modelled with WR stellar wind mass loss H/6 except $^{\rm *}$ which are done with H/3, $^{\rm R}$ indicates rotating models.
$M_{\rm 1,in}+M_{\rm 2,in}$ $p_{\rm in}$ $M_{\rm WR,5}$ $M_{\rm WR,1}$ p

$[{M}_{\odot}]$ $[\rm d]$ $[{M}_{\odot}]$ $[{M}_{\odot}]$ $\rm [d]$

41+20 6 11.8 11.2 12.6

$41+20^{\rm R}$ 6 11.0 10.2 9.8

41+24 6 12.1 11.4 21.5

$41+24^{\rm R}$ 6 11.2 10.5 16.4

$56+33^{\rm *}$ 6 18.6 17.5 13.8

$56+33^{\rm *,R}$ 6 14.9 13.6 8.5

**Table 4:** Comparison of resulting WR masses and orbital periods from non-rotating and rotating binary systems with the same initial parameters. $M_{\rm 1,in},M_{\rm 2,in}$ are initial primary and secondary mass, $p_{\rm in}$ is the initial orbital period, $M_{\rm WR,5}$ , $M_{\rm WR,1}$ are WR masses at $X_{\rm s}=0.05$ and $X_{\rm s}\le 0.01$ respectively and p is the orbital period in the initial WR+O system where the hydrogen surface abundance of WR star is $X_{\rm s}=0.05$ . Systems are modelled with WR stellar wind mass loss H/6 except $^{\rm *}$ which are done with H/3, $^{\rm R}$ indicates rotating models.
$M_{\rm 1,in}+M_{\rm 2,in}$	$p_{\rm in}$	$M_{\rm WR,5}$	$M_{\rm WR,1}$	p
$[{M}_{\odot}]$	$[\rm d]$	$[{M}_{\odot}]$	$[{M}_{\odot}]$	$\rm [d]$
41+20	6	11.8	11.2	12.6
$41+20^{\rm R}$	6	11.0	10.2	9.8
41+24	6	12.1	11.4	21.5
$41+24^{\rm R}$	6	11.2	10.5	16.4
$56+33^{\rm *}$	6	18.6	17.5	13.8
$56+33^{\rm *,R}$	6	14.9	13.6	8.5

Source LaTeX | All tables | In the text

	1 Introduction
	2 Observational data
	3 The simple approach
	4 Numerical code and physical assumptions
	5 Non-rotating models
	6 Rotating models
	7 Comparison with observations
	8 Conclusions
	References