Relationship between stellar spin-down during thermal relaxation and the degree of thermal disequilibrium at the time mass accretion ceases, for all models computed in this study. The spin-down is characterised by ω_TE/ω_crit, TE, where ω and ω_crit denote the surface and critical angular velocities, respectively, and the subscript “TE” refers to the time when TE is restored. The deviation from TE is quantified by (R_TE/R_T)^3/2, where R_T and R_TE are the stellar radii at the termination of accretion and at the restoration of TE, respectively. The exponent 3/2 arises from the dependence of the critical angular velocity on stellar radius (see Appendix A for details). Filled circles without gray edges represent single-star models from Set I, while filled markers with gray edges correspond to single-star models from other sets, with different markers denoting different sets, as is indicated in the legend. Open markers represent binary models, with the model number labeled beside. The color of each marker (or its edge color for binaries) indicates the mass accretion rate at the termination of accretion. The dashed black line indicates a linear relation with a slope of −1. The shaded gray and cyan regions indicate models that rotate rigidly and differentially, respectively, at the termination of accretion.