The figure shows the evolution of the virial ratio of star clusters under different models. (a) Virial ratio evolution for standard models with different initial masses and half-mass radii, as well as the binary model, all fluctuating around virial equilibrium. (b) Virial ratio evolution for models with increased maximum stellar mass, which also remain close to virial equilibrium. (c) Virial ratio evolution for power-law models, showing significant fluctuations in the early stage, indicating the quick dissolution of the system. (d) Virial ratio evolution for gas-expulsion models, exhibiting a strongly supervirial state at early times and rapidly declining to low values within a short timescale.