This PDF file includes:

• Materials and Methods
• Text
• Fig. S1. The nondimensionless planetesimal masses μ = ρ_p(δx)³ (here ρ_p is the particle density represented by the planetesimal in a grid cell and δx is the size of the cell) and corresponding contracted radii as a function of time after self-gravity is turned on.
• Fig. S2. The accretion radius R_acc (that is, the impact parameter required for accretion, given in units of the Bondi radius R_B) versus the particle friction time tf (in units of the Bondi time-scale t_B), for planetesimal radii R between 10⁻⁴ R_B and 10⁴ R_B.
• Fig. S3. The evolution of eccentricity e and inclination i of 1000 planetesimals with mass M = 1024 g located at 1 AU with a surface density of 10 g/cm², for three values of the time-step.
• Fig. S4. The evolution of eccentricity e and inclination i of 800 planetesimals with mass M = 1024 g located at 1 AU with a surface density of 10 g/cm².
• Fig. S5. Phase points covering planetesimal orbits with inclinations i = 0, i = 0.0016, i = 0.0032, and i = 0.0064.
• Fig. S6. The effect of eccentricity and inclination on the chondrule accretion rate, at an orbital distance of 2.5 AU.
  Fig. S7. The accretion rate of planetesimals at 25 AU, as a function of the planetesimal size.
• Fig. S8. The stratification integral (that is, the mean particle density over the accretion cross section) as a function of the accretion radius of the planetesimal.
• Fig. S9. The number of remaining bodies versus time for the constant kernel test.
• Fig. S10. Damping of eccentricities and inclinations of 10,000 1-cm–sized planetesimals located between 30 and 35 AU, emulating a test problem defined in Morbidelli et al. (21).
• Fig. S11. Cumulative size distribution after 3 Myr of coagulation within a population of planetesimals of initial diameters 100 km (50 km in radius), as shown by the cross.
• Fig. S12. Formation of planetesimals from centimeter-sized particles in a 2D shearing sheet simulation with the same spatial extent as the streaming instability simulations presented in the main text.
• References (56–77)

Download PDF