Fig. 2.

(A–C) The formation of a system of terrestrial planets. Each panel shows the mass of the planetesimals and planetary embryos as a function of semimajor axis, and color indicates their eccentricity. In addition, the error bars, which are only shown for objects larger than $0.01\hspace{0.17em}{M}_{\oplus }$ to decrease clutter, indicate the range of heliocentric distance that an object travels. The yellow box shows the region populated by planetesimals at $t=0$. (A) t = 2.0 Mya, (B) t = 23.0 Mya, and (C) t = 110.0 Mya. B shows the distribution of planetary embryos after pebble accretion but before the dynamical instability. C shows the final system. (D) The fiducial giant planet system constructed in ref. 6.