Period ratios of adjacent planetary pairs of all planets in the simulations (including the small bodies) after 3 Myr (end of the gas disc phase) and 100 Myr (dashed). In addition, we show the period distribution including only planets with masses larger than 0.5 Jupiter masses after 100 Myr (long-dashed lines). We do not observe a significant pile-up of planets close to mean-motion resonances, in contrast to the super-Earth simulations of Izidoro et al. (2019), which we attribute to the slower migration speed in the here used simulations, which prevents the formation of resonant chains at the inner edge of the protoplanetary discs. Nevertheless, the systems become unstable and the instabilities result in a wide spacing of the planets after 100 Myr.
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.