Growth and evolution of low-mass planets in pressure bumps

Open Access

Fig. 10

Left: planet mass, semimajor axis, and eccentricity as a function of time for runs in which the planet grows as a result of pebble accretion and for different values of the α viscosity and for St = 0.01. Right: same, but for different values of the Stokes number and for α = 10⁻⁴.

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