Ice-to-rock ratios in solar-system planets required to explain the solar compositional anomaly as a function of t_p, the time at which efficient planet formation starts and suppresses the accretion of rocks (metals) onto the star. The lines correspond to different values of the heat accretion parameter ξ = 0.5, 0.1 and 0, from top to bottom. Percentage figures (0–60%) indicate the fraction of rocks still in the accreting flow of the protosun for t ≤ t_p (100% corresponds to a rock-mass fraction equal to the protosolar value, 0.00489). The calculations assume M_Z,p = 150 M_⊕.