Overview of different BPS models.
|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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