Evolution of a 30 M_⊙ single star with a metallicity of Z_⊙/10, separated into different evolution phases. Dots indicate equal time intervals of 10⁵ years. The Hertzsprung gap is defined as the evolutionary stage between the terminal-age main sequence and the moment where the ratio of the nuclear burning luminosity and the surface luminosity satisfies |log₁₀(L_nuc/L)| < 0.001 for at least a thermal timescale estimated as GM²/RL, or the star develops a convective envelope > 1 M_⊙. Top: evolution under our default set of physical inputs. Middle: evolution with core overshooting increased from 0.335 to 0.535 pressure scale heights. Bottom: evolution with wind mass loss rates tripled.