Which stars can form planets: Planetesimal formation at low metallicities

Open Access

Fig. 2

Planetesimal formation in a turbulent disc. Top: evolution of pebble and planetesimal surface densities for a nominal turbulent viscosity of α_t = 10⁻³, a disc size of r_c = 100 au, and different values of disc metallicity. Bottom: evolution of the Stokes numbers and the corresponding midplane dust-to-gas ratios.

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