Mass loss from star clusters according to high-resolution N-body models by Berczik & Petrov (2008). The left panel shows the relative loss of the total mass of clusters orbiting at the solar galactocentric distance (R_G = 8.5 kpc). The solid (green), dotted (blue), and dashed (red) curves are for clusters of the initial masses M_c = 10³, 5  ×  10³, 10⁴   m_⊙, respectively. The right panel demonstrates selective mass loss occurring among stars of different masses m/m_⊙ in a cluster with M_c = 10³   m_⊙. The curves show the evolution of the MF-to-IMF ratio F(m,t)/f(m) with time, starting from t = 0 Myr, with a step of 100 Myr and last point t = 1249 Myr. The dots show the data of Anders et al. (2009) scaled to a cluster with mass M_c = 10³   m_⊙ and the age of 1249 Myr. The red portions of the curves correspond to stars alive and grey ones to stellar remnants.