Table B.1.
Literature predictions for WDNS and WDBH merger rates, R, based on the discussion of Toonen et al. (2018).
| R [yr−1] | |||
|---|---|---|---|
| Code/constraint | Reference | WDNS | WDBH |
| BPASS | This work | 1.4×10−5 | 1.8×10−7 |
| BSE | Shao & Li (2021) | - | < 3×10−6 |
| SeBa | Toonen et al. (2018) | (1-2)×10−4 | - |
| SeBaa | Nelemans et al. (2001) | 1.4×10−4 | 1.9×10−6 |
| Pulsar binaries | Bobrick et al. (2017) | 2.6×10−4 | - |
| X-ray binaries | Cooray (2004) | (1-10)×10−6 | - |
| WDNS binaries | Kim et al. (2004) | 4.1×10−6 | - |
| WDNS binaries | Davies et al. (2002) | 10−5 - 10−4 | - |
Notes. Population synthesis rates are provided above the horizontal line and, unless otherwise indicated, assume a constant star formation rate of 3 M⊙ yr−1. We provide BPASS merger rates at metallicity Z = 0.010 (by mass fraction). Merger rates derived from observed Galactic binary populations are listed below the line.
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