Can the giant planets of the Solar System form via pebble accretion in a smooth protoplanetary disc?

Open Access

Fig. A.7

Pebble accretion onset mass m_PA,hw in the headwind regime (solid line) and the planetesimal gravitational mass m_G (dashed line) at different locations of the disc r with the corresponding value of η shown in the upper x-axis. The values of m_G are around the mass range for the steep cutoff in k shown in Fig. A.6.

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