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Table E.1

AMD-stability coefficients computed for the systems affected by the MMR overlap criterion

Planet Period (d) Mass () Eccentricity β β (MMR)

HD 128311 Mass: 0.84

b 454.2 463.14 0.345 0.352 0.312
c 923.8 1032.46 0.230 0.244 3.200 27.931

HD 200964 Mass: 1.44

b 613.8 587.98 0.040 0.067 0.024
c 825 284.46 0.181 0.184 3.872 + ∞

HD 204313 Mass: 1.045

c 34.905 17.58 0.155 0.184 16.664
b 2024.1 1360.31 0.095 0.095 0.110 0.110
d 2831.6 533.95 0.280 0.308 8.032 + ∞

HD 33844 Mass: 1.75

b 551.4 622.94 0.150 0.180 0.084
c 916 556.20 0.130 0.189 2.939 22.676

HD 45364 Mass: 0.82

b 226.93 59.50 0.168 0.171 0.070
c 342.85 209.10 0.097 0.099 1.975 13.700

HD 47366 Mass: 1.81

b 363.3 556.20 0.089 0.138 0.146
c 684.7 591.16 0.278 0.292 2.896 2.896

HD 5319 Mass: 1.56

b 675 616.59 0.120 0.162 0.053
c 886 365.50 0.150 0.171 8.659 + ∞

HD 73526 Mass: 1.08

b 188.9 715.11 0.290 0.293 0.200
c 379.1 715.11 0.280 0.289 3.391 9.922

Notes. Masses are given in terms of nominal terrestrial masses and stellar masses in terms of nominal solar masses as recommended by the IAU 2015 Resolution B3 (Prša et al. 2016).

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