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Table 1.
Initial values and settings of key input physics parameters for the default and optimistic simulation, taken from Tables 2 and 8 of Kruckow et al. (2018).
| Name | Default simulation | Optimistic simulation |
|---|---|---|
| Number of simulated binaries, N | 109 | 109 |
| Initial mass function (IMF) parameter, αIMF | 2.7 (Salpeter 1955, Scalo 1986) | 2.3 (Kroupa et al. 2008) |
Primary mass,  |
∈[4 : 100] M⊙ | ∈[4 : 100] M⊙ |
| Mass ratio distribution | Kuiper (1935) | Kuiper (1935) |
Secondary mass,  |
∈[1 : 100] M⊙ | ∈[1 : 100] M⊙ |
| Period distribution | Öpik (1924), Abt (1983) | Öpik (1924), Abt (1983) |
| Semi-major axis, a | ∈[2 : 10 000] R⊙ | ∈[2 : 10 000] R⊙ |
| Eccentricity, e | 0 (initially circular orbit) | 0 (initially circular orbit) |
| Metallicity, Z | 0.0088 (Milky Way-like) | 0.0088 (Milky Way-like) |
| Rotation, vrot | 0 km s−1 (non-rotating stars) | 0 km s−1 (non-rotating stars) |
| During stable Roche-lobe overflow (RLO, Soberman et al. 1997): | ||
| Wind mass loss, αRLO | 0.2 | 0.15 |
| Minimum mass ejection by accretor, βmin | 0.75 | 0.5 |
| Circumbinary torus mass transfer, δRLO | 0 | 0 |
| Circumbinary torus size, γ | 2 | 2 |
| During CE: | ||
| CE efficiency parameter, αCE | 0.5 | 0.8 |
| Fraction of internal energy, αth | 0.5 | 0.3 |
| Critical mass ratio for mass transfer stability, qlimit | 2.5 | 2.5 |
Notes. The simulation at lower metallicity used the same parameters as the default simulation at Z = 0.0047.
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