Table 4
Inferred stellar and wind parameters.
| HMXB type | Persistent | Intermediate | SFXT | Persistent/ | Be X-ray | |
|---|---|---|---|---|---|---|
| Oe X-ray | ||||||
| Name | HD 153919 | BD+60 73 | LM Vel | HD 306414 | BD+53 2790 | HD 100199 |
| Spectral type | O6 Iafpe | BN0.7 Ib | O8.5 Ib-II(f)p | B0.5 Ia | O9.5 Vep | B0 IIIne |
| Alias name | 4U 1700-37 | IGR J00370+6122 | IGR J08408-4503 | IGR J11215-5952 | 4U 2206+54 | IGR J11305-6256 |
| T* [kK] |  |
 |
 |
 |
 |
 |
| T2∕3 [kK] | 34 | 23 | 29 | 24 | 30 | 30 |
| log g* [cm s−2] |  |
 |
 |
 |
 |
 |
| log L [L⊙] |  |
 |
 |
 |
 |
 |
| v∞∕103 [km s−1] |  |
 |
 |
 |
 |
 |
| β (a) |  |
 |
 |
 |
1.0 | 0.8 |
| R* [R⊙] |  |
 |
 |
 |
 |
 |
| R2∕3 [R⊙] | 20 | 18 | 17 | 31 | 11 | 6 |
| D |  |
 |
 |
 |
10 (b) | 10 (b) |
| log Ṁ [M⊙ yr−1] |  |
 |
 |
 |
 |
 |
| v sin i [km s−1] |  |
 |
 |
 |
 |
 |
| MV,John [mag] | − 6.4 | − 5.3 | − 5.8 | − 6.6 | − 4.7 | − 3.5 |
| XH [mass fr.] (c) |  |
 |
 |
 |
0.7375 | 0.7375 |
| XC∕10−3 [mass fr.] (c) |  |
 |
 |
 |
2.37 | 2.37 |
| XN∕10−3 [mass fr.] (c) |  |
 |
 |
 |
0.69 | 0.69 |
| XO∕10−3 [mass fr.] (c) |  |
 |
 |
 |
5.73 | 5.73 |
| XSi∕10−4 [mass fr.] (c) |  |
 |
 |
 |
6.65 | 6.65 |
| XMg∕10−4 [mass fr.] (c) | 6.92 |  |
 |
 |
6.92 | 6.92 |
| EB−V [mag] |  |
 |
 |
 |
 |
 |
| RV (reddening law (d)) | 3.1 (Seaton) |  (Cardelli) |
3.1 (Seaton) |  (Cardelli) |
3.1 (Seaton) | 3.1 (Seaton) |
| Mspec [M⊙] |  |
 |
 |
 |
 |
 |
| a2 [R*] |  |
 |
 |
 |
 |
– |
| vorb,apa [km s−1] |  |
 |
 |
 |
 |
– |
| vorb,peri [km s−1] |  |
 |
 |
 |
 |
– |
| vwind,apa [km s−1 ] |  |
 |
 |
 |
 |
– |
| vwind,peri [km s−1 ] |  |
 |
 |
 |
 |
– |
| Rrl,apa [R* ] (e) |  |
 |
 |
 |
 |
– |
| Rrl,peri [R* ] (e) |  |
 |
 |
 |
 |
– |
Notes. (a) Values larger than unity refer to the second exponent in a double-β law (see Sect. 4.1 for details). (b)We were not able to determine the precise clumping factor (see Appendix B for details). (c) Entries without errors are fixed to solar abundances (Asplund et al. 2009). (d) Seaton (1979); Cardelli et al. (1989). (e)Calculated via the approximation presented by Sepinsky et al. (2007), assuming the orbital parameters given in Table 2.
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