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Table 3

Stellar parameters of nine Of-type stars in N 206 superbubble.

N206-FS T ∗ log L log g∗ log Ṁ E B−V M V R ∗ ν∞ ν sin i M ∗ 1 log Q log Lmec4 Spectral type
# [kK] [L⊙] [cm s-2] [M⊙ yr-1] [mag] [mag] [R⊙] [km s-1] [km s-1] [M⊙] [s-1] [L⊙]
66 35.0 5.22 4.0 –6.38 0.17 –4.61 11.1 2200 67 45 48.7 2.22 O8 IV((f))
111 37.0 5.03 4.2 –6.85 0.10 –4.20 8.0 2500 43 37 48.6 1.86 O7 V((f))z
131a2 36.0 5.80 3.6 –5.50 0.11 –6.23 20.5 1500 96 61 49.4 2.77 O6.5 II(f)
131b3 30.0 5.04 3.8 –6.57 0.12 –5.00 12.3 1900 79 35 48.0 1.91 O9.7 IV
162 34.0 5.60 3.8 –6.03 0.20 –5.67 18.2 2100 83 77 49.1 2.53 O8 IV((f))e
178 35.0 5.22 4.0 –6.38 0.14 –4.55 11.1 2200 79 45 48.7 2.22 O7.5 III((f))
180a2 50.0 6.11 4.2 –5.32 0.16 –5.77 15.2 28007 128 133 50.0 3.49 O2 V((f*))
180b3 32.0 4.91 4.2 –6.62 0.18 –4.50 9.3 2900 42 50 48.0 2.21 O8 IV
1875 38.0 6.28 3.6 –4.80 0.19 –6.70 31.9 23007 116 148 50.0 3.86 O4 If
193 36.0 5.20 4.2 –6.36 0.20 –4.44 10.3 2900 103 61 48.7 2.48 O7 V((f))z
2146 38.0 6.10 3.6 –4.93 0.33 –6.26 26.0 23007 98 98 49.8 3.71 O4 If

Notes.

(1)

Spectroscopic masses.

(2)

Primary component.

(3)

Secondary component.

(4)

The mechanical luminosity .

(5)

When strong clumping (D = 20 and RD = 0.05 R∗) is adopted then log Ṁ = −5.59 M⊙ yr-1 and log Lmec = 3.05 L⊙. The X-ray field is included in this model, with X-ray luminosity LX = 4.7 × 1033 erg s-1.

(6)

When strong clumping (D = 20 and RD = 0.05 R∗) is adopted then log Ṁ = −5.72 M⊙ yr-1 and log Lmec = 2.92 L⊙. The X-ray field is included in this model, with X-ray luminosity LX = 1.7 × 1033 erg s-1.

(7)

ν∞ is determined from UV P-Cygni profiles. Other values are theoretically calculated from νesc.

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