Evolution of equatorial surface rotational velocity of a single 24 M_⊙ star for different values of initial rotational velocity by assuming the formalism of the Vink et al. (2001) stellar wind model (solid lines) and the Björklund et al. (2023) wind model (dashed lines). In addition, tracks without the Spruit – Tayler dynamo mechanism (dotted-dashed lines) and the tracks assumed Fuller et al. (2019) AM transport (dotted lines) are added for reference. The tracks represent only the main-sequence stage up to terminal-age evolutionary phase. The error bars represent the observed position of HD 46485, whose primary has comparable mass.