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Fig. 21

image

Left panel: radial velocities right after gas expulsion and at a cluster age around 6 Myr as a function of Mecl. The simulations are for clusters with εSFE = 0.33 and initial HMR of 0.3 pc. They consider stellar evolution, no primordial mass segregation and no Galactic tidal field, one simulation per mass. Right panel: evolution of Lagrange radii for a 105M cluster (this time not in logarithmic scale, resulting in a clear visibility of only the outermost radii) to explain the acceleration of the outer layers: at a cluster age around 3.8 Myr, stellar evolution causes noticeable mass loss. The outer low density regions have not yet slowed down from the initial expansion due to gas expulsion, because the stars have little chance to interact. Further mass loss through stellar evolution can therefore not be compensated, resulting in an accelerated expansion.

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