Description


Compact objects were formed as follows:



Evolution of bound mass and cluster radius:

Figures

  1. 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).
  2. Fig.2 shows the evolution of the lagrangian radii. Plotted radii show the fraction of enclosed mass.
  3. 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.
  4. 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.
  5. 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.