Primordial segregation in globular clusters: The degree of mass segregation as determined through dynamical models

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Fig. B.2

Normalized half-mass radius as function of stellar mass for N = 50 000 generated stars (black circles) with the corresponding theoretical prediction (green line) for models with $Φ_{0} = 0.01 M_{⊙}^{- 1}$ $Mathematical equation: ${{\rm{\Phi }}_0} = 0.01{\rm{ M}}_ \odot ^{ - 1}$$ (upper panel) and $Φ_{0} = 0.1 M_{⊙}^{- 1}$ $Mathematical equation: ${{\rm{\Phi }}_0} = 0.1{\rm{ M}}_ \odot ^{ - 1}$$ (lower panel), adopting a double power law mass function with slope α₁ = −1.3 for 0.1 ≤ m/M_⊙ < 0.5 and α₂ = −2.3 for 0.5 ≤ m/M_⊙ ≤ 100.

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