Which stars can form planets: Planetesimal formation at low metallicities

Open Access

Fig. 7

Disc turbulence dependence of planetesimal formation at the water-ice line in a disc with r_c = 100 au and [Fe/H] = 0. Top: time evolution of the total solid mass without planetesimal formation taking place in the disc. Bottom: time evolution of the dust and pebble mass, including planetesimal formation in the disc.

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