Table 6
CE and nebula ejection reconstruction parameters for a sample of post-CE PNe.
| Nebula | α | Menv | fM | ΔEorb | Ebin,neb | Ekin,neb | fE | References |
|---|---|---|---|---|---|---|---|---|
| (M⊙) | (erg) | (erg) | (erg) | |||||
| Single-degenerate post-CE PNe | ||||||||
| Abell 63 | 0.29 | 1.7 | 1% | 1.4 × 1047 | 8.3 × 1044 | 5 × 1043 | 0.6% | de Marco et al. (2008), Iaconi & De Marco (2019) |
| Hen 2-155 | 0.3 | 1.7 | 22% | 1.4 × 1047 | 9.7 × 1045 | 2.9 × 1045 | 9% (a) | Jones et al. (2015), Iaconi & De Marco (2019) |
| Double-degenerate post-CE PNe | ||||||||
| Fg 1 | 0.11 (b) | 0.7 | 64% | 1.4 × 1047 (b) | 1 × 1046 | 5.9 × 1045 | 11% | Boffin et al. (2012) |
| Hen 2-428 | 0.04 | 1.1 | 61% | 4 × 1047 | 9.8 × 1045 | 1.6 × 1045 | 3% | Reindl et al. (2020) |
Notes. Columns represent CE ejection (whole envelope) efficiency α, AGB envelope mass Menv, percentage of envelope mass each nebula represents, fM, orbital energy budget, ΔEorb, rough estimate of the observednebula binding energy, Ebin,neb, observed nebula kinetic energy, Ekin,neb, and percentage of the energy budget spent on unbinding and accelerating the nebula, fE. (a) Characteristic expansion velocity unavailable; average expansion velocity of SD systems has been used (see Table B.1). (b) Mass of the secondary star (in the range 0.7–1 M⊙ according to radial velocity analysis, and in the range 0.63–0.7 M⊙ according to evolutionary and ionisation considerations) assumed to be 0.7 M⊙.
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