Formation of planetary systems by pebble accretion and migration - Hot super-Earth systems from breaking compact resonant chains

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Table 2

Selected setups to model the formation and long-term dynamical evolution of close-in super-Earths based on the results of Sect. 3.

Scenarios	t_start	S_peb	I_peb (M_⊕)





Model-I	0.5 Myr	1	~194
Model-I	3.0 Myr	5	~150
Model-II	3.0 Myr	5	~150
Model-III	0.5 Myr	10	~1940

Notes. From left to right, the columns are name of the model, disk age at the start of the simulation (t_start), the scaled pebble flux (S_peb), and the integrated pebble flux (I_peb). In our nominal simulations, Rocky_peb = 0.1 cm but we also performed simulations with Rocky_peb = 1 cm.

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