Description
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Coordinates and masses taken from the example-file at http://www.maths.ed.ac.uk/people/douglas/kyotoii/ic.dat.gz
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20480 stars in total.
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Binaries treated as inert therefore effectively 16384 single stars
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No stellar evolution
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Tidal cut-off
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Total computing time: 5.5 hours on GRAPE6
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Total energy error: 0.5 %
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Scaling relations from N-body units to length, mass, speed, time:
| R* |
6.4026 pc |
| M* |
10174.27 M_sun |
| V* |
2.6138 km/s |
| T* |
2.3995 Myr |
Results
Evolution of bound mass:
| T(Myr) |
N |
M/M0 |
Rhalf(pc) |
| 0.00 |
16384 |
1.0000 |
5.43 |
| 200.00 |
15877 |
0.9756 |
5.81 |
| 400.00 |
14848 |
0.9116 |
6.70 |
| 600.00 |
13574 |
0.8432 |
7.20 |
| 800.00 |
12235 |
0.7755 |
7.61 |
| 1000.00 |
10838 |
0.7126 |
7.57 |
| 1200.00 |
9194 |
0.6302 |
8.27 |
| 1400.00 |
7514 |
0.5518 |
8.12 |
| 1600.00 |
5445 |
0.4459 |
8.16 |
| 1800.00 |
3380 |
0.3295 |
7.77 |
| 2000.00 |
1612 |
0.2077 |
6.26 |
| 2200.00 |
424 |
0.0982 |
4.75 |
Figures
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Fig.1 shows the evolution of the number of cluster
stars and the bound mass-fraction. The Mass-fraction is shown by the dotted
line.
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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 anisotropy-profile
at four different times and for different mass-groups. The dissolution
time was defined to be T = 2500 Myr.