Table 1
Percentage of binaries in each residence times category for all the cases studied in this article.
| Cat. 1 | Cat. 2 | Cat. 3 | Figure | |
|
|
||||
| Planar Circular-Neptune case | ||||
| Non-resonant and eCM = 0 | 51.8 | 1.2 | 47.0 | 4, 10 |
| Resonant and eCM = 0 | 52.8 | 2.9 | 44.3 | 4 |
| Resonant and eCM = 0.3 | 69.7 | 7.3 | 23.0 | 10 |
|
|
||||
| Planar Eccentric-Neptune case | ||||
| Non-resonant and eCM = 0 | 52.8 | 1.7 | 45.5 | 5, 11 |
| Resonant and eCM = 0 | 52.4 | 1.5 | 46.1 | 5 |
| Resonant and eCM = 0.3 | 70.3 | 5.6 | 24.1 | 11 |
|
|
||||
| Non-planar Circular-Neptune case | ||||
| Non-resonant and eCM = 0 | 81.3 | 5.3 | 13.4 | 13 |
| Resonant and eCM = 0.3 | 89.8 | 4.7 | 5.5 | 13 |
Notes.The first category corresponds to binaries which exit the Hill sphere in less than 2000 years, the second one to binaires staying coupled between 2000 and 20 000 years and the last one to asteroids which remain inside the Hill sphere for 20 000 years or longer. The number of the figures related to these data is also given.
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