tokens: T icb = 6.36 × 10 4 K; the density ρ icb = 1.47 g cm −3 . The composition is uniform with 100% silicates out to a temperature T = 2.1 × 10 4 K and radius 2.72 × 10 9 cm, decreasing to 50% at T = 5.42 × 10 3 K and radius 3.39 × 10 9 cm, and to 1% at T = 2960 K and radius 4.84 × 10 9 cm. During the isolated phase, the parameter in Equation ( 7 ) is set to 0.04. During the first 10 8 yr, an additional 0.25 M ⊕ is lost, giving M XY = 0.42 M ⊕ , R p = 7.43 R ⊕ , L = 2.0 × 10 −10 L ⊙ , and a cooling time of 8 × 10 8 yr. At this time, M ⊕ yr −1 . As in Run 0.128 (Rev), a radiative zone extends inward to T = 1500 K. Later, the luminosity declines to ≈10 −11 L ⊙ , the cooling time increases by an order of magnitude and the rate of mass loss declines significantly, by a factor of 400, to 2 × 10 −12 M ⊕ yr −1 , by the final time. Between t = 10 8 yr and t = 7 × 10 9 yr, a further 0.13 M ⊕ is lost from the H/He envelope. The radius of the final model planet agrees quite well with that of the actual planet, as does the total mass. The total heavy-element mass (including the inner and outer cores) is M Z = 7.52 M ⊕ , and the H/He mass M XY = 0.29 M ⊕ . The inner core of 1.87 M ⊕ has R icore = 1.075 R ⊕ and mean density 8.35 g cm −3 . The region of almost 100% heavy elements has radius 1.84 R ⊕ , and the mean density of the inner plus outer cores is 5.86 g cm −3 . The mass of this final model is very close to that of the in situ model 0.128 (Rev). The temperature at the boundary between the inner and outer cores ( T icb ) is similar (1.54 × 10 4 K versus 1.75 × 10 4 K), and the corresponding density is slightly lower (7.59 versus 8.0 g cm −3 ). These differences are presumably caused primarily by the different masses of the inner cores. Both final models have outer radiative zones, extending inward to T = 1850 K in the in situ case and to 1500 K in the present case; they include less than 1% of the envelope mass. The structure of the final model for Run 1.00 (Rev) is plotted in Figure 12 . Figure 12. Structure of the model in Run 1.00 (Rev) at time 7.03 × 10 9 yr. Symbols and curves: as in Figure 11 . The mean density of the inner core is 8.35 g cm −3 . 3.4. Migration Model: Run 1.00(Old) Run 1.00(Old) starts at 1 au with σ init = 190 g cm −2 , slightly lower than that in Run 1.00(Rev). Outer densities and temperatures are the same in the two runs. The masses and radius as a function of time are given in Figure 13 . At first, M core increases very rapidly until, at t ≈ 7 × 10 3 yr, it reaches 6.78 M ⊕ , close to the isolation mass of 6.81 M ⊕ . At this point, M env = 0.084 M ⊕ . The temperature T cb is 9.91 × 10 3 K, much lower than the value of T icb = 6.1 × 10 4 K reached at a comparable evolutionary phase in Run 1.00 (Rev). The lower mean molecular weight in the H/He envelope accounts for much of this difference. The luminosity during the solid accretion phase averages about 10 −4 L ⊙ , corresponding to a mass accretion rate onto the core of 1 to 1.5 ×
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