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Table 2

Inferred stellar parameters for the SMC WR binaries.

AB3 AB5 AB6 AB7 AB8
Component A B A B C A B A B A B

Spectral typea WN3h O9 WN6h WN6-7 O WN4 O6.5 I WN4 O6 I(f) WO4 O4 V
T [kK]
T2 / 3 [kK]
log g [cm s-2]b 4.3 3.5 3.5 3.7 4.7 5.1
log L [L]
log Rt [R]
v/ 103 [km s-1]
R [R]
R2 / 3 [R]
D 10 40-20 10 10 10 10 40-20 10
log [M yr-1]c −8.0 −5.9 −5.8
vsini [km s-1] <300 < 400
veq [km s-1]d <300 < 400
MV,John [mag]
XH (mass fr.)e 0.25 0.73 0.25 0.25 0.73 0.4 0.73 0.15 0.73 0+ 0.15 0.73
XC/ 10-5 (mass fr.)e 21 21 21 21 21
XN/ 10-3 (mass fr.)e 0.03 ( | 1) f 0.03 0.03 ( | 0.3) f 0.03 ( | 0.3) f 0 0.03
XO/ 10-5 (mass fr.)e 5.5 110 5.5 5.5 110 5.5 110 5.5 110 110
EBV [mag] 0.18 0.08 0.065 0.08 0.07
AV [mag] 0.56 0.25 0.20 0.25 0.22
MH−b [M]g
MHe−b [M]g
Mg [M]
Morb [M]h
RRL [R] i

Notes. All entries but spectral types, Morb, and RRL are derived in this study unless otherwise stated. Values without errors are adopted.

(a)

References as in Table 1.

(b)

Fixed for WR components using Morb and R (see Sect. 4.3).

(c)

Unconstrained entries adopted from Vink et al. (2000).

(d)

Equatorial rotation velocity calculated assuming alignment of the orbital and rotational axes.

(e)

Entries without errors are fixed to typical SMC abundances (see Sect. 4.2).

(f)

Alternative values in parentheses obtained when assuming the N iiiλ4640 emission originates in the O component (see Appendix A).

(g)

Obtained from MLRs by Gräfener et al. (2011) (see Sect. 6.1).

(h)

Based on orbital parameters given in Table 1.

(i)

Calculated via the Eggleton approximation (Eggleton 1983) assuming the orbital parameters given in Table 1.

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