Table 3
Initial conditions for the computed model clusters without a gas expulsion phase (see Sect. 2.1).
| Mcl(0) /M⊙ | rh(0)/pc | Primordial binaries | Stellar evolution | Mass segregation | V∗(0)/ km s-1 | τcr(0)/Myr | τh(0)/Myr |
|
|
|||||||
| 104 | 0.3 | no | yes | no | 10.5 | 0.028 | 4.65 |
| 3 × 104 | 0.3 | no | yes | no | 18.1 | 0.017 | 8.05 |
| 104 | 1.0 | no | yes | no | 5.8 | 0.172 | 28.30 |
| 3 × 104 | 1.0 | no | yes | no | 10.0 | 0.100 | 49.02 |
| 105 | 1.0 | no | yes | no | 18.2 | 0.055 | 89.49 |
| 1.3 × 104 | 0.35 | yes | yes | yes | 11.7 | 0.030 | 6.68 |
| 104 | 1.0 | yes | yes | yes | 6.0 | 0.167 | 28.30 |
| 3 × 104 | 1.0 | yes | yes | yes | 10.4 | 0.096 | 49.02 |
Notes. The initial configurations are Plummer profiles with total mass, Mcl(0) and half-mass radius rh(0). The corresponding values of the virial velocity dispersion (velocity dispersion within the virial radius ≈ rh(0)), V∗(0); the crossing time, τcr(0) = rh(0) /V∗(0); and the two-body relaxation time at half-mass radius, τh(0), are given. Also indicated is whether the initial system includes primordial binaries (see Sect. 2.1) and whether it is mass segregated (as in Baumgardt et al. 2008). Stellar evolution (see Sect. 2.1) is used in all N-body calculations. The initial clusters are always located at RG ≈ 8 kpc Galactocentric distance (the solar distance) and they orbit the Galactic center with VG ≈ 220 km s-1.
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