Simulated angular velocity evolutions of 1.0 M_⊙ stars with initial rotation periods at 5 Myr of 1 (upper curve), 2, 3, 6, 10, and 20 days (lower curve). Left: the simulated angular velocity curves in log-log scale are compared with rotation measurements of 0.9–1.1 M_⊙ stars (black crosses) in the Pleiades (112 Myr; Hartman et al. 2010), M50 (130 Myr; Irwin et al. 2009), M35 (133 Myr; Meibom et al. 2009), and M37 (550 Myr; Hartman et al. 2009). Right: the simulated angular velocity curves in linear scale are compared with rotation measurements of 0.9–1.1 M_⊙ stars (black crosses) in M37, NGC 6811 (1.05 Gyrs; Meibom et al. 2011), NGC 6819 (2.38 Gyrs; Meibom et al. 2015), and M67 (4.0 Gyrs; Barnes et al. 2016).