Evolutionary tracks computed for HD 75332. The scenarios without (solid lines) and with (dashed line) the engulfment of a 3 M_J planet at an initial orbital distance a_in = 0.025 AU are included. For the stellar initial surface rotation rate, we considered values of Ω_in(Ω_⊙) = 3.2, 5.0, 18, as representative of the evolution as slow, moderate and fast rotator (Eggenberger et al. 2019). The spike featured by the dashed line indicates the effect the planetary engulfment has on the stellar property. In the top-left panel, the black dot shows the observed surface rotation rate as in Brown et al. (2021). In the top-right panel, the black dots shows the estimates of angular momentum loss derived by using the prescription in Finley & Matt (2018) and the values in Table 2 of Brown et al. (2021). The gray square shows the mean value of the angular momentum loss estimates multiplied by a factor 20. In the bottom-left panel, the back dot shows the observational value of the X-ray luminosity from Vidotto et al. (2014a). In the bottom-right panel, the black dot shows the semi-empirical angular momentum obtained by multiplying the best-fit stellar model momentum of inertia by the surface rotation rate in Brown et al. (2021).