Table 1
Percentage of simulated particles with a< 2.5 AU and q> 1.8 AU that are below the g = g6 secular resonance line for each run seperately, for particles of all runs combined, as well as the percentage of the real asteroids with radii H< 9 and H< 10.
| Simulation | % below g = g6 | % below g = g6 | % below g = g6 |
| (i ≤ 20°) | (t = 200 Myr) | ||
|
|
|||
| run1 | 3.54 | 4.55 | 7.69 |
| run2 | 3.15 | 2.83 | 0.00 |
| run3 | 2.31 | 1.89 | 0.00 |
| run4 | 7.64 | 8.62 | 23.81 |
| run5 | 2.94 | 1.25 | 0.00 |
| run6 | 4.35 | 4.63 | 15.00 |
| run7 | 1.68 | 1.06 | 0.00 |
| run8 | 5.08 | 5.15 | 9.09 |
| run9 | 6.15 | 6.86 | 0.00 |
| run10 | 2.36 | 2.27 | 0.00 |
| total | 4.00 | 4.07 | 8.44 |
| real H< 9 | 93.88 | ... | ... |
| real H< 10 | 93.42 | ... | ... |
Notes. The third column lists the percentages for asteroids with initial inclinations i ≤ 20° and the fourth column lists those modified after 200 Myr of evolution.
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