Figure 4:

Effects of temperature, oxygen fugacity, and timing of initial differentiation on the mantle ¹⁸²W anomaly (red circles and lines) and f^Hf/W (blue triangles and lines) for one example Earth analogue, with simultaneously varying equilibration depths chosen to match the mantle W abundance. Left panel: Results of changing the equilibration temperature, expressed as a deviation from the liquidus of Andrault et al. (2011). Center panel: Results of changing the initial oxygen fugacity at which embryo and planetesimal compositions are calculated at the start of the model. Right panel: Results of changing the time at which embryos and planetesimals first differentiate with respect to the Hf–W system, either at the onset of the N-body simulation (solid line) or when they experience their first impact (dotted line) (e.g., Nimmo and Agnor, 2006), the effects of which are a function of the fraction of incoming metal that equilibrates, k. Labels indicate the depth of equilibration, expressed as a fraction of the core–mantle boundary pressure. Equilibration with three times the impactor’s silicate mass, k = 0.4, and initial oxygen fugacity of IW–3.5 were used except as noted.