Evolution of average angle θ of star-disk spin with respect to the spin after t = 1.2 Myr (upper panel) and t = 0.5 Myr (lower panel) for various upper and lower limits of the stellar masses. The average angle is computed based on stars that have an age of more than 1.2 Myr at the end of the simulation. Upper panel: Mean average relative angle of orientation with respect to the orientation at t = 1.2 Myr for stars with masses of M_*(1.2 Myr) less than 0.2 M_⊙, 1 M_⊙, and 2 M_⊙, shown as light to dark purple lines. Dark to light green lines mark the mean average angle of orientation with respect to the orientation at t = 1.2 Myr for stars with final masses greater than 0.2 M_⊙, 1 M_⊙, and 2 M_⊙. Lower panel: Average mean angle of orientation with respect to the orientation at t = 1.2 Myr for stars with masses in the mass ranges of M_* (1.2 Myr) < 0.2 M_⊙, 0.2 M_⊙ < M_*(1.2 Myr) < 1 M_⊙, 1 M_⊙ < M_*(1.2 Myr) < 2 M_⊙, and M_*(1.2Myr) > 2 M_⊙, shown as light to dark blue lines. The upper panel can be directly compared with the results presented in Kuffmeier et al. (2023), while the evolution for mass ranges shown in lower panel is arguably more helpful for comparison with observations of various stellar types.