Table 5
Summary of dusty WC binary properties (upper panel) and remaining X-ray detected binaries (lower panel).
| WR | Spectral type | Porb | LX | Period determinations | Reference |
| (1033 erg s-1) | |||||
|
|
|||||
| 77n/W239 | WC9vd+? | 5.053 ± 0.002 day | 0.4 | RV | This work |
| Clark et al. (2008) | |||||
| 19 | WC4pd + O9.6 | 10.1 yr | – | photometric | Veen et al. (1998) |
| 48a | WC8ed + ? | ~ 1 yr + > 30 yr? | 100 | photometric (provisional) | Williams et al. (2003) |
| Zhekov et al. (2010) | |||||
| 65 | WC9d+? | “few years” | 0.1 | variable X-ray | Oskinova & Hamann (2008) |
| 70 | WC9vd + B0 I | 1045 ± 60 day | – | photometric | Williams et al. (2008) |
| 98a | WC8-9vd + ? | 564 ± 8 day | – | photometric + imaging | Monnier et al. (1999) |
| Williams et al. (2003) | |||||
| 104 | WC9pd + B0.5 V | 241.5 ± 0.5 day | – | imaging | Tuthill et al. (2008) |
| Crowther (1997) | |||||
| 112 | WC9d + ? | 24.8 ± 1.5 yr | – | imaging (provisional) | Marchenko et al. (2002) |
| 113 | WC8d+O8-9IV | ~ 29.707 day | – | RV | Massey & Niemela (1981) |
| 118 | WC9d + ? | ~ 60 day | – | imaging (provisional) | Millour et al. (2007) |
| 125 | WC7ed + O9 III | > 4 yr | – | photometric (provisional) | Williams et al. (1994) |
| 137 | WC7ed + O9 | 13.05 ± 0.15 yr | – | RV + photometric | Williams et al. (2001) |
| Lefevre et al. (2005) | |||||
| 140 | WC7pd +O4-5 | 7.94 ± 0.03 yr | 5–12 | RV + photometric | Williams et al. (1990) |
| Pollock et al. (2005) | |||||
| Zhekov & Skinner (2000) | |||||
| HD 36402 | WC4(+O?)+O8 I | 3.03269 | – | RV | Moffat et al. (1990) |
| Williams (2011) | |||||
|
|
|||||
| 11 | WC8+O7.5III | 78.53 ± 0.01 day | 1.2–1.5 | RV | Schmutz et al. (1997) |
| Schild et al. (2004) | |||||
| 48 | WC5+O9.5/B0Iab | 19.138 ± 0.003 day | 1.0 | RV | Hill et al. (2002) |
| (WC6+O6V) | Oskinova (2005) | ||||
| 79 | WC7+O5V | 8.8911 ± 0.0001 day | 0.05 | RV | Hill et al. (2000) |
| Oskinova (2005) | |||||
Notes. Column 5 summarises the origin of the orbital period, being derived from Radial Velocity data, periodicities in the photometric lightcurve, the motion of a pinwheel nebula (imaging) and/or a variable X-ray flux. In several cases (WR48a, 65, 112, 118 & 125) these are less robust and so are labeled as provisional. RV variations are also present in WR70 and are consistent with both short (~50 d) and long (~1200 d) periods. Note the discrepant classifications given for WR48 in Hill et al. (2002) and Oskinva (2005). Nazé (2009) report an X-ray detection of the WC7+O7/9 binary WR93 but no X-ray flux is given.
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