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 Ṁ[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 |
| EB−V [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.
References as in Table 1.
Fixed for WR components using Morb and R∗ (see Sect. 4.3).
Unconstrained entries adopted from Vink et al. (2000).
Entries without errors are fixed to typical SMC abundances (see Sect. 4.2).
Alternative values in parentheses obtained when assuming the N iii λ4640 emission originates in the O component (see Appendix A).
Obtained from MLRs by Gräfener et al. (2011) (see Sect. 6.1).
Based on orbital parameters given in Table 1.
Calculated via the Eggleton approximation (Eggleton 1983) assuming the orbital parameters given in Table 1.
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