Table 1
Stellar masses, periods P, and eccentricity e of the analysed DWDs at the end of the second CE, and respective progenitors.
| M1 [M⊙] | M2 [M⊙] | P [h] | e | Δt | Teff 1 [K] | Teff 2 [K] | Mz1 | Mz2 | Pz | ez | |
|---|---|---|---|---|---|---|---|---|---|---|---|
| DWD1 | 0.60 | 0.38 | 20.47 | 0 | 135 Gyr | 8600 | 75 000 | 2.6 | 1.9 | 172 days | 0 |
| DWD2 | 0.21 | 0.31 | 0.43 | 0 | 9 Myr | 20400 | 58 400 | 1.55 | 1.25 | 1.13 days | 0 |
 |
0.75 | 0.26 | 1.51 | 0 | 150 Myr | 8800 | 52000 | 3.47 | 1.95 | 52 yr | 0.98 |
 |
0.31 | 0.25 | 1.71 | 0 | 430 Myr | 8100 | 50100 | 1.84 | 1.28 | 83.5 days | 0.68 |
Notes. The subscript Z indicates the stellar mass and period at the ZAMS; subscripts 1 and 2 refer to the primary and the secondary star, respectively. At is the time needed for the merging of the two DWDs computed via Eq. (9) of Danielski et al. (2019). Teff 1 and Teff 2 are the effective temperatures of the WDs immediately after the second CE. The period P corresponds to the period of the DWD binary just after the second CE. The systems marked with an asterisk (*) belong to the LISA DWD population presented in Korol et al. (2019). More details can be found in Sect. 2.1.
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