Open Access
Table 1
Initial conditions of the star-cluster models.
| Object type | Stars | Common features | ffc models with Q=0.25, 0.5, and 0.75 |
|---|---|---|---|
| Model name for each ffcs subset | C025 & C05 & C075 | ||
| Number of objects | 10000 | 30000 | |
| Number of stars in binaries, nbin | 1000 | ||
| Object initial mass function | (1), 0.08–150 M⊙ | Equal mass, mffc=10−11 M⊙ | |
| Total mass, Mcl | 6.62 × 103 M⊙ | 3 × 10−7 M⊙ | |
| Density profile | (2) | ||
| Objects spatial distribution | Virial distribution | Statistically subvirial & identical & supervirial compared to stars | |
| ffc velocity distribution | Virial distribution | Statistically subvirial & identical & supervirial compared to stars | |
| Half-mass radius, rhm | 1 pc | ||
| Virial radius | 1.3 pc | ||
| General characteristics | |||
| N-body (Hénon) time unit, T* | 0.27 Myr | ||
| Crossing time, tcr | 0.25 Myr | ||
| Half-mass relaxation time, trh | 40.63 Myr | ||
| Stellar evolution (3) | Mass loss enabled | ||
| External tidal force | Solar neighborhood | ||
| Simulation time | 1000 Myr |
Notes. Each cluster model is named based on the value of the virial ratio of the ffc population. The stellar component is the same in all models; only the ffcs population changes energy distribution. (1) Kroupa (2001b); (2) Plummer (1911); (3) Kamlah et al. (2022).
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