Table 2.
Models with simplified stellar evolution and without SG stars run in this work.
| Model (a) | W0 | rh | Segregation | Number of particles | Softening length | fmass loss |
|---|---|---|---|---|---|---|
| (pc) | (pc) | |||||
| n7Ne | 7 | 23 | N | 25 600 | 1.65 | 0.63 |
| n7Ye | 7 | 23 | Y | 25 600 | 1.65 | 0.74 |
| n5Ne | 5 | 37 | N | 25 600 | 2.57 | 0.70 |
| n5Ye | 5 | 37 | Y | 25 600 | 2.57 | 0.79 |
| n2Ne | 2 | 60 | N | 25 600 | 4.20 | 1.00 |
| n2Ye | 2 | 60 | Y | 25 600 | 4.20 | 1.00 |
| N2Ne | 2 | 60 | N | 102 400 | 2.65 | 1.00 |
Notes. The initial mass of each simulated cluster is M0 = 8.4 × 106 M⊙, after the removal of 16% of its mass.
Model name: n or N = small or large number of particles + W0 + N or Y = non-segregated or segregated + e = with stellar evolution. Columns: same as in Table 1.
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