Table 1.
List of properties of selected LC18 progenitors that lead to successful explosions and also form a black hole.
| Progenitor | ξ2.0 | tfin | ![]() |
![]() |
![]() |
Eexpl |
|---|---|---|---|---|---|---|
| (s) | (M⊙) | (M⊙) | (km) | (B) | ||
| 060b300 | 0.65 | 0.92 | 2.45 | 2.07 | 7449 | 2.06 |
| 080b000 | 0.58 | 0.35 | 2.54 | > 2.08 | 629 | 0.00 |
| 080b300 | 0.60 | 0.59 | 2.49 | > 2.08 | 2762 | 0.18 |
| 080c000 | 0.58 | 0.64 | 2.49 | > 2.08 | 2586 | 2.22 |
| 080d000 | 0.57 | 0.53 | 2.50 | > 2.08 | 2357 | 2.21 |
Notes. In the first column, the name of the progenitor indicates its ZAMS mass in M⊙ (first three characters), metallicity (a, b, c, and d stands for z⊙, 10−1 z⊙, 10−2 z⊙, and 10−3 z⊙, respectively), and initial rotation in km/s (last three characters). The remaining columns are the compactness (defined in Eq. (7), the final time post bounce tfin when the simulation stops (i.e. very close to BH formation), the final baryonic mass of the PNS
, the gravitational mass of the cold neutron star
corresponding to
, the maximum shock radius
reached during the simulation, and finally the explosion energy Eexpl at the end of the simulation defined in Eq. (6).
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