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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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