Fig. 5
Number of resonances covering the period ratios space for equal-mass planets, with masses 10−5 M⊙. At first order, the number of resonances can be compared to the filling factor ρtot (Eq. (58)). We plot the two-planet circular Hill-stability limits (Petit et al. 2018) for both planet pairs in green and the predicted overlap limit for the three-planet MMRs (Eq. (59)) in blue.
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