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Fig. 2

image

Planetary mass-semimajor axis distribution at the simulation time of 0.1 Myr for a solar metallicity disc with different combinations of a disc’s viscosity parameter α and an initial disc age tinit. Here, tinit = 0.1 and 0.5 Myr correspond to the inital t = 0 and 0.4 Myr, respectively, in Eq. (4). The green, pink, and orange lines indicate the snow line, the boundary between viscous and irradiation regimes, and the boundary between Stokes and Epstein regimes, respectively. Each panel shows the results from five simulations as blue circles, and grey squares represent the corresponding parameters for planets observed by the radial velocity method. A peak and a jump seen in mass growth can be explained by different regimes of the disc (see text).

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