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Home All issues Volume 672 (April 2023) A&A, 672 (2023) A198 Full HTML
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Table 1.

Stellar and optical depth parameter τwind of binary and single WN stars in the LMC with a surface-hydrogen mass fraction of XH ≥ 0.40.

BAT99 Spectral type log L T* R* υ∞ log Ṁ XH τwind Porb Mcomp/MWR
# [L⊙] [kK] [R⊙] [km s−1] [M⊙ yr−1] [d]
Binary
006 O3 If*/WN7 5.90 45 15.0 1800 −5.60 0.70 0.10 2.0
072 WN4 5.05 70 2.3 1800 −5.50 0.40 0.70
077 WN7 5.79 45 13.0 1000 −5.20 0.70 0.47 3.0 1.66 ± 0.20
079 WN7 5.90 45 15.0 1000 −4.60 0.40 1.34
107 O6.5 Iafc 6.09 33 34.0 1300 −5.20 0.70 0.15 153.9 0.81 ± 0.02
113 O2 If*/WN5 6.14 47 18.0 1800 −5.50 0.70 0.11 4.7 0.32 ± 0.04
116 (a) WN5h 6.43 53 19.0 2500 −4.20 0.65 1.53 154.5 0.92 ± 0.07
119 WN6h 6.35 50 20.0 1200 −4.40 0.40 1.38 158.7 1.01 ± 0.05
Single
012 O2 If*/WN5 5.80 50 10.6 2400 −5.53 0.50 0.12
068 O3.5 If*/WN7 6.00 45 16.7 1000 −5.46 0.60 0.19
081 WN5h 5.48 47 8.2 1000 −5.55 0.40 0.27
093 O3 If* 5.90 45 14.9 1600 −5.63 0.60 0.10
097 O3.5 If*/WN7 6.30 45 23.7 1600 −5.18 0.60 0.18
098 WN6 6.70 45 37.5 1600 −4.43 0.60 0.63
102 WN6 6.80 45 42.1 1600 −4.21 0.40 0.82
103 WN5(h) 6.25 47 19.9 1600 −4.70 0.40 0.56
104 O2 If*/WN5 6.06 63 9.0 2400 −5.34 0.40 0.20
105 O2 If* 6.40 50 21.1 1600 −5.41 0.60 0.18
106 WN5h 6.51 56 19.0 2400 −4.55 0.40 0.60
108 WN5h 6.87 56 28.8 2400 −4.43 0.40 0.52
109 WN5h 6.69 56 23.4 2400 −4.56 0.40 0.47
110 O2 If* 6.22 50 17.1 2400 −5.22 0.70 0.17
111 WN9ha 6.25 45 22.3 1000 −5.42 0.70 0.17
114 O2 If*/WN5 6.44 63 13.9 2400 −5.35 0.40 0.13
117 WN5ha 6.40 63 13.3 2400 −4.93 0.40 0.36
130 WN11h 5.68 28 29.1 200 −5.35 0.40 0.40
133 WN11h 5.69 28 29.4 200 −5.42 0.40 0.33

Notes. The stellar parameters of the binary and single WN (and O) stars are taken from Shenar et al. (2019, 2020b) and Hainich et al. (2014) respectively. The stellar bolometric luminosity, temperature and radius are given by L, T* and R*. The terminal wind speed and surface hydrogen mass fraction is given by υ∞ and XH. The wind mass-loss rate of the WN star is given by Ṁ. The orbital period and mass ratio (mass of companion divided by mass of WN star) of the binary systems are given by Porb and q, respectively, whenever available (Shenar et al. 2019). We quote the mass ratios for the WR binaries for which Shenar et al. (2019) found SB2 solutions, but not from the spectroscopic masses reported in Table 2 of Shenar et al. (2019).

(a)

Parameters adopted from Tehrani et al. (2019).

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