Table 1.
Properties of the known long-period binaries with either confirmed or candidate high-mass WDs and AFGK-type main-sequence stars, ordered according to their orbital periods.
| System | Orbital period | WD mass | Companion mass | Eccentricity | Reference |
|---|---|---|---|---|---|
| (d) | (M⊙) | (M⊙) | |||
| Low-eccentricity systems | |||||
| J2117+0332 | 17.9239 ± 0.0001 | > 1.244 ± 0.027 | 1.11 ± 0.03 | 0.0007 ± 0.0002 | (4) |
| IK Peg | 21.7217 ± 0.0001 | 1.13 − 1.24 | ∼1.7 | ∼0 | (1, 2, 3) |
| J1111+5515 | 32.1494 ± 0.0022 | > 1.367 ± 0.028 | 1.15 ± 0.02 | 0.0217 ± 0.0003 | (4) |
| J1314+3818 | 45.5150 ± 0.0047 | 1.324 ± 0.037 | 0.71 ± 0.01 | 0.0503 ± 0.0003 | (4) |
| J2034−5037 | 46.1147 ± 0.0006 | > 1.418 ± 0.033 | 0.96 ± 0.02 | 0.0079 ± 0.0002 | (4) |
| J0107−2827 | 49.0063 ± 0.0008 | > 1.271 ± 0.030 | 0.97 ± 0.03 | 0.0901 ± 0.0005 | (4) |
| High-eccentricity systems | |||||
| TYC 5451−469−1( * ) | 203.5757 ± 0.1247 | > 0.938 ± 0.248 | 1.04 ± 0.47 | 0.2045 ± 0.0044 | (5) |
| J0353+2900( * ) | 1484.344 ± 134.116 | 1.117 ± 0.164 | 1.95 ± 0.13 | 0.3452 ± 0.0410 | (5) |
Notes. Systems marked with an asterisk( * ) have high eccentricities, most likely descend from initial triple systems, and therefore do not provide constraints on CE evolution.
References. (1) Landsman et al. (1993), (2) Vennes et al. (1998), (3) Lucy & Sweeney (1971), (4) Yamaguchi et al. (2024), (5) Garbutt et al. (2024).
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