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Figure 1: Projected rotational ( left panel) and macro-turbulent ( right panel) velocities of OB-SGs (spectral types refer to O-stars, i.e., 10 corresponds to B0 and 20 to A0). Data derived in the present study are marked with diamonds while crosses refer to published data (Simon-Diaz & Herrero 2007; Dufton et al. 2006). |
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Figure 2:
Effects of micro-turbulence on the strength of Si IV 4116/Si III 4553
(left panel) and Si II 4128/Si III 4553 (right panel) equivalent width
ratios for B-type SGs.
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Figure 3:
Examples for the quality of our final (``best'') Silicon
line-profile fits. From top to bottom: HD 185859 (B0.5Ia), HD 190603
(B1.5Ia+), HD 206165 (B2Ib) and HD 198478 (B2.5Ia). Note the systematic
discrepancy between synthetic and observed profiles of the Si III lines at
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Figure 4:
Observed and synthetic helium line-profiles, calculated at the upper
(
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Figure 5:
Final (``best'') fits to Silicon and helium lines. From top to
bottom: HD 198478 (B2.5), HD 191243 (B5Ib), HD 199478 (B8ae),
HD 212593 (B9 Iab) and HD 202850 (B9 Iab). Note that the forbidden
component in the blue wing of He I ![]() ![]() |
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Figure 6:
Fit quality for H![]() ![]() |
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Figure 7: As for Fig. 6, but for late B subtypes. From top to bottom: HD 191243 (B5Ib), HD 199478 (B8ae), HD 212593 (B9Iab) and HD 202850 (B9Iab). |
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Figure 8:
Left: comparison of effective temperatures as derived in the
present study with data from similar investigations. Diamonds - our data;
triangles - data from Crowther et al. (2006); squares - Urbaneja (2004);
asterisks - Przybilla et al. (2006). Large circles mark the three
objects with strongest winds, which simultaneously show the largest
deviation in
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Figure 9:
Differences between ``unblanketed'' and ``blanketed'' effective temperatures
for the combined sample (this work; Urbaneja 2004; Crowther et al. 2006;
Przybilla et al. 2006 and GROUP I objects from Lefever et al. 2007), as a
function of spectral type ( left panel) and as a function of ![]() ![]() ![]() |
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Figure 10:
Temperature scale for Galactic B-SG as derived in the present study
(dashed, see text), compared to
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Figure 11:
Left: WLR for Galactic
B-SGs, based on data from the combined sample: diamonds - our data;
triangles - data from Crowther et al. (2006); squares - data from Urbaneja (2004)
and plus signs - data from Lefever et al. (2007) (GROUP I, without the three
``problematic'' objects). The two pairs of symbols connected with dashed
lines correspond to the two entries for HD 190603 and HD 198478 as
listed in Table 2. For the latter object and for HD 199478, we
also provide error bars indicating the rather large uncertainty in their
wind-momenta. Specially marked objects are discussed in the text.
Right: wind-momenta of B-SGs from the left (diamonds and asterisks) are
compared with similar data for O-SGs (triangles). Filled diamonds indicate
B-type objects with
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Figure 12:
Ratio of ![]() ![]() ![]() ![]() |
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Figure 13:
Modified optical depth invariant, ![]() ![]() |
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Figure 14:
Wind-efficiency, ![]() ![]() |
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