Comparisons of four models of Earth formation by rapid pebble accretion to the Hf-W isotope data for Earth. The top panels (Model 1) shows results for our nominal impactor mass of 0.4 M_E colliding with proto-Earth after 40 Myr. The excess of ¹⁸²W in the mantle builds up a to a value of nearly 10 before the interaction of the mantle material with the impacting Theia core delivers enough ¹⁸³W to bring the є_W value down towards the measured data. The second panel (Model 2) show instead the effect of lowering the impactor to 0.185 M_E (we use here our Venus analogue for the proto-Earth model). We set the impact to occur after 60 Myr to avoid subsequent build up of ¹⁸²W in the mantle, but the impactor mass is too low to bring the model to agree with the measured є_W of Earth. The canonical impactor model is reconciled with the Hf-W system in the third row (Model 3) where we include two giant impacts: an early impact at 20 Myr removes the initial ¹⁸²W excess and the second (moon-forming) giant impact brings the subsequent mantle ingrowth of ¹⁸²W down to the modern terrestrial value. Finally, the lower panels (Model 4) show the effect of lowering the equilibration efficiency to f_eq = 0.5. The є_W value ends above the terrestrial value in this case.