Table 2
Ionizing flux emitted from our models of stripped stars.
| Z | LHI/Ltot | LHeI /Ltot | LHeII/Ltot | log 10Q0_st (red-enh) | log 10Q1_st (red-enh) | log 10Q2_st (red-enh) | |||
| [s-1] | [s-1] | [s-1] | |||||||
|
|
|||||||||
| 0.02 | 0.853 | 0.602 | 1.8 × 10-8 | 48.1 | (48.1–48.1) | 47.8 | (47.8–47.8) | 40.1 | (44.7–39.3) |
| 0.0166 | 0.854 | 0.604 | 4.6 × 10-8 | 48.1 | (48.1–48.1) | 47.8 | (47.8–47.8) | 40.5 | (44.8–39.3) |
| 0.0142 | 0.854 | 0.605 | 1.2 × 10-7 | 48.1 | (48.1–48.1) | 47.8 | (47.8–47.8) | 40.9 | (44.8–39.3) |
| 0.0134 | 0.853 | 0.604 | 1.5 × 10-7 | 48.1 | (48.1–48.1) | 47.8 | (47.8–47.8) | 41.1 | (44.9–39.3) |
| 0.01 | 0.853 | 0.605 | 5.1 × 10-7 | 48.1 | (48.1–48.1) | 47.9 | (47.9–47.9) | 41.6 | (44.9–39.3) |
| 0.005 | 0.847 | 0.599 | 2.8 × 10-6 | 48.2 | (48.2–48.2) | 47.9 | (47.9–47.9) | 42.4 | (44.9–39.4) |
| 0.0047 | 0.846 | 0.597 | 3.0 × 10-6 | 48.2 | (48.2–48.2) | 47.9 | (47.9–47.9) | 42.4 | (44.9–39.4) |
| 0.0021 | 0.828 | 0.573 | 2.8 × 10-4 | 48.2 | (48.2–48.2) | 48.0 | (48.0–48.0) | 44.4 | (44.8–40.3) |
| 0.001 | 0.798 | 0.535 | 4.3 × 10-4 | 48.3 | (48.3–48.3) | 48.0 | (48.0–48.0) | 44.7 | (44.5–41.4) |
| 0.0005 | 0.746 | 0.471 | 2.9 × 10-4 | 48.3 | (48.3–48.3) | 48.0 | (48.0–48.0) | 44.5 | (44.2–41.7) |
| 0.0002 | 0.681 | 0.395 | 2.1 × 10-5 | 48.3 | (48.3–48.3) | 48.0 | (48.0–48.0) | 43.4 | (43.1–43.9) |
| 0.0001 | 0.613 | 0.329 | 1.2 × 10-5 | 48.3 | (48.3–48.3) | 47.9 | (47.9–47.9) | 43.2 | (43.0–43.7) |
Notes. Cols. 2–4 show the fraction of the emitted luminosity that is HI, HeI, and HeII ionizing, respectively. The last three columns show the number of ionizing photons emitted per second from each model. In parenthesis we show the values for the reduced and enhanced mass loss rate models of the given metallicity. Our reference models are marked with gray background.
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