Table 1
Stellar masses, periods, binary separations, and critical semimajor axis of the three analyzed DWDs.
| System | M1 (M⊙) | M2 (M⊙) | Pbin (h) | abin (au) | acrit (au) |
|---|---|---|---|---|---|
| DWD2 | 0.31 | 0.21 | 0.43 | 1.078 × 10−3 | 2.36 × 10−3 |
 |
0.75 | 0.26 | 1.51 | 3.106 × 10−3 | 6.82 × 10−3 |
 |
0.31 | 0.25 | 1.71 | 2.773 × 10−3 | 6.06 × 10−3 |
Notes. The binary eccentricity is zero for all the systems (see Ledda et al. 2023, their Table 1 for more details). The inclinations are set to zero for simplicity. The systems marked with the * belong to the LISA DWD population presented in Korol et al. (2019). acrit is calculated with Eq. (5).
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