Description
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Cluster set-up is the same as in run6 except:
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Stellar evolution, which was modeled by implementing the routines of Hurley et al. 2000,
MNRAS 315, 543
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Binaries were treated as inert, only stellar evolution of the components was made
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Total computing time: 10.5 hours on GRAPE6
Results
Compact objects were formed as follows:
Black holes |
Neutron stars |
ONe White Dwarfs |
CO White Dwarfs |
6 |
54 |
22 |
1002 |
Evolution of bound mass and cluster radius:
T(Myr) |
N |
M/M0 |
Rhalf(pc) |
0.00 |
16384 |
1.0000 |
5.43 |
500.00 |
14958 |
0.7741 |
6.62 |
1000.00 |
13299 |
0.6794 |
6.69 |
1500.00 |
11531 |
0.5920 |
6.60 |
2000.00 |
9629 |
0.5065 |
6.56 |
2500.00 |
7590 |
0.4224 |
6.14 |
3000.00 |
5695 |
0.3412 |
5.82 |
3500.00 |
3869 |
0.2571 |
5.51 |
4000.00 |
2380 |
0.1788 |
4.60 |
4500.00 |
1207 |
0.1074 |
4.07 |
5000.00 |
531 |
0.0580 |
2.94 |
5500.00 |
136 |
0.0189 |
2.56 |
Figures
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Fig.1 shows the evolution of the number of cluster
stars (solid), the fraction of bound mass (short dashed) and the mass lost
due to stellar evolution (long dashed).
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Fig.2 shows the evolution of the lagrangian radii.
Plotted radii show the fraction of enclosed mass.
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Fig.3 shows the evolution of the mean stellar mass
for different lagrangian shells. The dotted line shows the average mass
of all stars in the cluster.
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Fig.4 shows the evolution of the mass fraction in
different components. Main sequence and giant stars are splitted into two groups, high and
low-mass stars. The dividing line is close to m = 0.7 Msun.
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Fig.5 shows the mass distribution of MS and giant stars at the
start of the simulation and when (from top to bottom) 30%, 60% and 90% of the lifetime are over.