(O–Mg–2Si)/Fe vs. Mg/Si and (O–Mg–2Si)/Fe versus Fe/Mg plots for the sample of the simulated planets around four different stars. The dashed black lines divide the planets into different types predicting different interior properties. On the left, Mg/Si = 1.0 is the division between more pyroxene-rich (Mg/Si < 1.0) and olivine–pyroxene mixed (Mg/Si > 1.0) mantles. On the right, the Fe/Mg = 0.9 line separates the planets with potentially smaller cores (Fe/Mg < 0.9) and potentially bigger cores (Fe/Mg > 0.9). Above the horizontal line at (O–Mg–2Si)/Fe = 1, the planets are expected to be more oxidized, and below typically less oxidized. The values for the Earth (Wang et al. 2018) and Mars (Yoshizaki & McDonough 2020) are shown for reference. The planetesimal formation time of 0.8 Myr is assumed here.