Table 3
Overview of different BPS models.
| Model | Description | Reference | |
|
|
|||
| Star formation history | BP | Star formation rate and space density depends on time and location | 1 |
| in the Galaxy. SFR peaks at early times, declines afterwards | |||
| cSFR | Constant space density and SFR for 10 Gyr | – | |
|
|
|||
| Initial period distribution | Abt | Log-uniform | 2 |
| Lognormal | Lognormal distribution with a mean of 5.03 d | 3 | |
|
|
|||
| Common-envelope phase | γα | γ = 1.75, αλ = 2; Preferred for unresolved DWDs | 4, 5, 6 |
| αα | αλ = 2 | 4, 6 | |
| αα2 | αλ = 0.25; Preferred for unresolved WDMS | 7, 8, 9 | |
Notes. There are two models for the SFH, two for the period distribution, and three for the CE-phase, giving 12 models in total. 1Boissier & Prantzos (1999); 2Abt (1983); 3Raghavan et al. (2010); 4Nelemans et al. (2000); 5Nelemans et al. (2001b); 6Toonen et al. (2012); 7Zorotovic et al. (2010); 8Toonen & Nelemans (2013); 9Camacho et al. (2014).
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