The mass distribution of stars stripped in binaries: The effect of metallicity

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Table 1.

Estimated numbers of binary-stripped stars.

M_strip	Metallicity (Z_*)
(M_⊙)	0.014	0.006	0.002	0.0002
1 − 50	27788 ± 173	29594 ± 180	32126 ± 182	34766 ± 190
> M_drop		5 ± 2	119 ± 12	213 ± 13
> M_WR^(a)	560 ± 22	211 ± 14	11 ± 4

1 − 1.4	14733 ± 133	15533 ± 119	17168 ± 140	18207 ± 122
1.4 − 2.6	9044 ± 87	9865 ± 94	10655 ± 104	12473 ± 108
2.6 − 5	2579 ± 46	2743 ± 50	2913 ± 61	3204 ± 62
5 − 10	912 ± 30	968 ± 32	1067 ± 30	589 ± 24
> 10	301 ± 16	253 ± 14	63 ± 9	3 ± 2

Notes. The estimates shown are for a population in equilibrium and in which stars form at a constant rate of 1 M_⊙/yr.

^(a)

The M_WR values are the $M_{spec, He}^{WR}$ $M_{\mathrm{spec, He}}^{\mathrm{WR}}$ values obtained by Shenar et al. (2020): 7.5, 11, and 17 M_⊙ at Z = 0.014, 0.006, and 0.002, respectively.

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