Linking planetary embryo formation to planetesimal formation - I. The effect of the planetesimal surface density in the terrestrial planet zone

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Table 1

Analytic embryo formation model extrapolation until 10 Myr from the systems of Figs. 2–4.

Total mass	Σ_P profile	T₀ at 2 au	T₀ at 3 au	T₀ at 4 au
6 M_⊕	Σ_P ∝ r^−1.0	2.26 Myr	5.06 Myr	9.47 Myr
6 M_⊕	Σ_P ∝ r^−1.5	2.2 Myr	5.76 Myr	>10 Myr
6 M_⊕	Σ_P ∝ r^−2.0	2.35 Myr	7.16 Myr	>10 Myr

13 M_⊕	Σ_P ∝ r^−1.0	1.21 Myr	2.63 Myr	5.02 Myr
13 M_⊕	Σ_P ∝ r^−1.5	1.19 Myr	3.02 Myr	6.48 Myr
13 M_⊕	Σ_P ∝ r^−2.0	1.26 Myr	3.77 Myr	9.03 Myr

27 M_⊕	Σ_P ∝ r^−1.0	0.73 Myr	1.45 Myr	2.72 Myr
27 M_⊕	Σ_P ∝ r^−1.5	0.72 Myr	1.65 Myr	3.53 Myr
27 M_⊕	Σ_P ∝ r^−2.0	0.75 Myr	2.05 Myr	4.98 Myr

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