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Table 2
Cluster models, resulting mean cluster densities and age, at which these densities are reached in the leaky cluster development.
| No. of stars | Mean density | Cluster age | Encounter |
| M⊙/ pc3 | Myr | probability | |
|
|
|||
| 32 000 | 4.2 × 104 | – | – |
| 16 000 | 2.1 × 104 | – | 63.4% |
| 8000 | 1.0 × 104 | – | 41.9% |
| 4000 | 5.3 × 103 | 1.8 Myr | 28.4% |
| 2000 | 2.7 × 103 | 2.3 Myr | 21.3% |
| 1000 | 1.3 × 103 | 2.8 Myr | 16.9% |
Notes. The last column shows the probability for a solar-type star located within 0.7 pc from the center to ungergo an encounter between 100 AU and 1000 AU.
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