Angular-momentum luminosity ﹩\langle {{ \mathcal L }}_{J}\rangle ﹩ (black solid line) as a function of fractional stellar radius for the primary TOI-5882. To ensure consistency with Figures 2 and 3, these profiles are computed using the same stellar model, forced at the model-predicted orbital period of P_orb ≈ 5.95 days. The right panel shows the GYRE-tides calculation with only radiative damping, while the left panel includes both radiative and viscous damping. The blue shaded region represents the gravitational component of the luminosity ﹩{\langle {{ \mathcal L }}_{J}\rangle }_{{\rm{grav}}}﹩ and the red shaded region shows the wave component ﹩{\langle {{ \mathcal L }}_{J}\rangle }_{{\rm{wave}}}﹩. The horizontal dashed line marks the surface value of ﹩\langle {{ \mathcal L }}_{J}\rangle ﹩, which is equal and opposite to the net torque ﹩\langle { \mathcal T }\rangle ﹩ on the star. The hatched region shows the convective zone of the star and the orange shaded zone represents the hydrogen-burning shell.