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Home All issues Volume 703 (November 2025) A&A, 703 (2025) A131 Full HTML
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Table B.1.

Number of ionizing photons predicted by our models in the Lyman, He I and He II continua, as well as the predicted hardness ratio I4686/IHβ = A⋅Q(He II)/Q(H I), explained in Sect. 3.2.

D = 1 (smooth wind) D = 10 (clumped wind, for reference)
star [M⊙] log Ṁ log Teff log L L ⊙ $ \log \frac{L}{L_\odot} $ log QH I log QH I log QHe II I4686/IHβ log QH I log QHe I log QHe II I4686/IHβ
20-0.28 [20] -8.5 4.58 4.68 48.23 47.50 41.91 < 0.01 48.18 47.32 42.03 < 0.01
20-0.5 [20] -7.8 4.65 4.97 48.70 48.20 43.88 < 0.01 48.68 48.16 43.77 < 0.01
20-0.75 [19.8] -6.9 4.74 5.29 49.12 48.74 44.66 < 0.01 49.11 48.73 44.66 < 0.01
20-0.98 [19.2] -5.8 4.88 5.58 49.45 49.19 46.87 < 0.01 49.45 49.19 45.10 < 0.01
20-pMS [16.8] -5.5 5.08 5.67 49.47 49.32 48.52 0.20 49.50 49.34 48.61 0.22
59-0.28 [58.9] -7.0 4.74 5.75 49.58 49.20 45.59 < 0.01 49.57 49.20 45.25 < 0.01
59-0.5 [58.7] -6.7 4.79 5.94 49.80 49.46 46.26 < 0.01 49.79 49.45 45.74 < 0.01
59-0.75 [58.3] -5.8 4.84 6.13 50.00 49.71 47.22 < 0.01 49.99 49.70 46.79 < 0.01
59-0.98 [55.3] -4.7 4.92 6.29 50.08 49.94 49.31 0.30 50.10 49.95 49.24 0.24
59-pMS [49.4] -4.7 5.14 6.34 50.06 49.94 49.44 0.42 50.09 49.95 49.32 0.30
131-0.28 [130.8] -6.2 4.76 6.29 50.14 49.78 46.79 < 0.01 50.14 49.77 46.24 < 0.01
131-0.5 [129.9] -5.9 4.79 6.42 50.28 49.95 47.19 < 0.01 50.28 49.94 46.58 < 0.01
131-0.75 [126.8] -4.9 4.84 6.57 50.45 50.15 48.12 < 0.01 50.44 50.15 46.10 < 0.01
131-0.98 [112.5] -4.27 4.93 6.69 50.53 50.32 49.23 0.09 50.53 50.32 48.95 0.05
131-e-pMS [106.7] -4.09* 5.14* 6.70* 50.42* 50.32* 49.80* 0.42* − − − −
131-m-pMS [101.8] -4.16* 5.14* 6.69* 50.42* 50.31* 49.79* 0.41* − − − −
131-(l)-pMS [93.3] -4.23 5.14 6.68 50.41 50.26 49.71 0.35 50.46 50.27 49.55 0.21
Models with reduced mass loss, see Paper II (for reference only, not used in population synthesis)
20-0.28 -10.5 same as above 48.24 47.52 41.81 < 0.01 48.19 47.34 40.84 < 0.01
20-0.5 -9.8 48.70 48.20 43.84 < 0.01 48.68 48.16 42.41 < 0.01
20-0.75 -8.9 49.12 48.74 45.48 < 0.01 49.11 48.73 43.75 < 0.01
20-0.98 -7.8 49.45 49.19 46.66 < 0.01 49.44 49.19 46.09 < 0.01
20-pMS -7.5 49.48 49.32 48.48 0.17 49.49 49.32 48.41 0.14
59-0.28 -9.0 49.58 49.20 45.67 < 0.01 49.57 49.20 44.62 < 0.01
59-0.5 -8.7 49.80 49.46 46.13 < 0.01 49.79 49.45 44.96 < 0.01
59-0.75 -7.8 49.99 49.71 46.71 < 0.01 49.99 49.70 45.86 < 0.01
59-0.98 -6.7 50.11 49.96 49.19 0.21 50.13 49.96 49.11 0.17
59-pMS -6.7 50.09 49.96 49.39 0.35 50.10 49.97 49.34 0.30
131-0.28 -8.2 50.14 49.78 46.59 < 0.01 50.14 49.77 46.44 < 0.01
131-0.5 -7.9 50.28 49.95 46.84 < 0.01 50.28 49.94 45.34 < 0.01
131-0.75 -6.9 50.44 50.15 47.60 < 0.01 50.44 50.14 46.75 < 0.01
131-0.98 -6.27 50.55 50.32 48.91 0.04 50.55 50.31 48.57 0.02
131-pMS -6.23 50.43 50.30 49.74 0.36 50.44 50.31 49.71 0.32

Notes. Models marked with * are newly computed for this work. Population synthesis is performed on QH I and QHe II separately (see Sect. 2.3) to arrive at the final hardness ratio reported in Table 1 which is representative for the whole population. For convenience, we list basic stellar parameters such as actual mass [M⊙], mass-loss rate [M⊙ yr−1], log Teff/K and log L/L⊙ (also to be found in Paper II, except for the new models); these are taken from the evolutionary models and used as input for the PoWR atmosphere code (see the HR diagram in Fig. 1). The sets with reduced mass loss and a high wind clumping are here for reference; in the population synthesis, we use the models with nominal mass-loss rates and smooth winds.

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