Table 1
Selected properties of our He-core pre-WD sequences.
| M ⋆ /M ⊙ |
|
M H / M ⊙ | τ instability |
| [ 10-3 ] | [yr] | ||
|
|
|||
| 0.1554 | 0.365 | 4.34 | 1.9 × 109 |
| 0.1612 | 0.376 | 4.19 | 1.3 × 109 |
| 0.1650 | 0.390 | 4.09 | 1.1 × 109 |
| 0.1706 | 0.405 | 3.94 | 4.1 × 108 |
| 0.1762 | 0.423 | 3.80 | 2.5 × 108 |
| 0.1822 | 0.440 | 3.66 | 1.6 × 108 |
| 0.1869 | 0.453 | 3.55 | 1.4 × 108 |
| 0.1921 | 0.466 | 3.42 | 5.8 × 107 |
| 0.2026 | 0.490 | 3.22 | 6.5 × 107 |
| 0.2390 | 0.701 | 2.86 | 3.4 × 107 |
| 0.2724 | 0.715 | 2.02 | – |
Notes.The table lists the stellar mass, the H surface abundance, the mass of the H content at the point of maximum Teff at the beginning of the first cooling branch, and the time it takes the models to evolve along the instability domain (thick blue lines in Fig. 1) in the nondiffusion computations.
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