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Table B.3

Results for dry rocky planets observed by TESS after 30,000 runs (Monte Carlo method).

Exoplanet Mp Rp S:O Prot a D2 D3 Seff Prob. CMF MMF Roℓ Regime /
GJ 1252 b 2.119 ±0.311 1.190 ± 0.042 1:1 0.518 0.009 0.144 0.282 234.7 0.94 0.47 ± 0.20 0.53 ± 020 0.03 ± 0.01 Dipolar 3.50 ± 1.40
GJ 3473 b 1.965 ±0.135 1.252 ± 0.025 1:1 1.198 0.016 0.124 0.245 59.2 0.54 0.15 ±0.10 0.85 ±0.10 0.14 ± 0.03 Multip. 0.05 ± 0.02
GJ 357 b 1.884 ±0.171 1.202 ± 0.043 1:1 3.931 0.034 0.129 0.252 13.5 0.77 0.29 ± 0.16 0.71 ± 0.16 0.47 ± 0.09 Multip. 0.04 ± 0.02
GJ 367 b 0.546 ± 0.045 0.718 ± 0.031 1:1 0.322 0.007 0.182 0.343 588.2 1.00 0.92 ± 0.015 0.08 ± 0.015 0.01 ± 0.002 Dipolar 0.86 ±0.38
HD 15337 b 7.547 ± 0.607 1.640 ± 0.035 1:1 4.756 0.053 0.644 1.201 160.9 1.00 0.48 ± 0.10 0.52 ±0.10 0.37 ± 0.07 Multip. 0.33 ±0.15
HD 213885 b 8.835 ±0.379 1.744 ± 0.030 1:1 1.008 0.020 1.067 1.939 3420 1.00 0.39 ± 0.07 0.61 ± 0.07 0.07 ± 0.01 Dipolar 12.59 ± 1.50
HD 21749 c 0.670 ± 0.038* 0.886 ±0.031 1:1 7.790 0.069 0.458 0.823 41.4 0.84 0.36 ± 0.16 0.64 ± 0.16 1.03 ± 0.21 Multip. 0.01 ± 0.002
L 168-9 b 4.600 ± 0.323 1.390 ±0.052 1:1 1.402 0.021 0.259 0.512 157.7 1.00 0.64 ± 0.13 0.36 ±0.13 0.04 ± 0.01 Dipolar 9.11 ± 1.09
LHS 1478 b 2.330 ±0.116 1.243 ± 0.029 1:1 1.950 0.019 0.088 0.173 20.3 1.00 0.40 ±0.11 0.60 ±0.11 0.15 ±0.03 Multip. 0.17 ± 0.08
LHS 1678 b 0.350 ± 0.000 0.696 ± 0.025 3:2 0.573 0.012 0.130 0.242 98.0 1.00 0.60 ± 0.13 0.40 ± 0.13 0.05 ± 0.01 Dipolar 0.64 ±0.03
LHS 1678 c 1.400 ± 0.000 0.983 ± 0.037 1:1 3.694 0.032 0.124 0.242 13.9 1.00 0.77 ± 0.12 0.23 ± 0.12 0.15 ±0.03 Multip. 0.14 ± 0.01
LHS 1815 b 1.356 ± 0.077* 1.085 ± 0.036 1:1 3.814 0.038 0.205 0.396 27.6 0.96 0.34 ± 0.16 0.66 ± 0.16 0.42 ± 0.08 Multip. 0.04 ± 0.02
LHS 3844 b 2.295 ± 0.127* 1.302 ±0.012 1:1 0.463 0.006 0.054 0.108 71.2 0.95 0.17 ± 0.08 0.83 ±0.08 0.04 ± 0.01 Dipolar 1.53 ± 0.69
LP 791-18 b 1.508 ± 0.086* 1.093 ± 0.061 1:1 0.948 0.010 0.046 0.093 20.8 0.79 0.44 ± 0.23 0.54 ± 0.23 0.07 ± 0.01 Dipolar 2.01 ± 0.96
LTT 3780 b 2.681 ± 0.257 1.323 ± 0.040 1:1 0.768 0.012 0.126 0.250 103.8 0.86 0.29 ± 0.15 0.71 ±0.15 0.06 ± 0.01 Dipolar 2.97 ± 1.34
TOI-1235 b 5.992 ± 0.342 1.677 ± 0.038 1:1 3.445 0.038 0.294 0.577 60.1 0.72 0.17 ± 0.10 0.83 ± 0.10 0.42 ± 0.08 Multip. 0.10 ±0.04
TOI-1444 b 3.871 ±0.408 1.397 ± 0.037 1:1 0.470 0.012 0.760 1.388 4838 1.00 0.46 ± 0.14 0.54 ± 0.14 0.03 ± 0.01 Dipolar 6.59 ± 1.32
TOI-1749 c 14.00 ± 0.00 2.069 ± 0.040 1:1 4.493 0.044 0.260 0.509 34.7 0.58 0.14 ± 0.08 0.86 ± 0.08 0.57 ±0.11 Multip. 0.15 ±0.01
TOI-178 b 1.589 ± 0.196 1.141 ± 0.039 1:1 1.915 0.026 0.368 0.689 192.6 0.67 0.31 ±0.17 0.69 ± 0.17 0.20 ± 0.04 Multip. 0.07 ± 0.03
TOI-2285 b 19.50 ±0.00 1.740 ± 0.046 3:2 18.180 0.137 0.168 0.338 1.6 1.00 0.92 ± 0.06 0.08 ± 0.06 0.48 ± 0.10 Multip. 0.57 ± 0.03
TOI-270 b 1.677 ± 0.109 1.198 ± 0.021 1:1 3.360 0.032 0.144 0.281 19.0 0.56 0.15 ± 0.09 0.85 ± 0.09 0.46 ±0.09 Multip. 0.02 ±0.01
TOI-431 b 3.069 ±0.202 1.280 ± 0.023 1:1 0.490 0.011 0.504 0.935 2112 1.00 0.57 ± 0.08 0.43 ± 0.08 0.02 ± 0.004 Dipolar 5.86 ± 1.17
TOI-540 b 0.699 ± 0.039* 0.899 ± 0.028 1:1 1.239 0.012 0.062 0.120 23.1 0.90 0.35 ±0.15 0.65 ± 0.15 0.12 ±0.02 Dipolar 0.75 ± 0.30
TOI-700 b 1.143 ± 0.065* 1.034 ±0.036 1:1 9.977 0.067 0.156 0.304 5.0 0.95 0.34 ± 0.16 0.66 ± 0.16 1.30 ±0.26 Multip. 0.02 ±0.01
TOI-700 d 1.620 ± 0.092* 1.144 ± 0.035 1:1 37.425 0.163 0.155 0.304 0.87 0.98 0.33 ±0.15 0.67 ± 0.15 5.66 ± 0.94 Multip. 0.01 ± 0.002

Notes. Mp is the planetary mass normalized to the Earth mass. Those values highlighted with an asterisk have been estimated following (Chen & Kipping 2017). Rp is the planetary radius normalized to the Earth radius. S:0 shows the Spin:Orbit resonance. Prot is the planetary rotational period in days, a, D2 and D3 are respectively are the semi-major axis, inner and outer boundaries of the HZ expressed in A.U. Seff is normalized mean effective flux considering orbital eccentricity. Prob. It is the probability of being rocky planet. All the planets are tidally locked. Errors in the rotational period have not been included because they are so small that they have no impact on the magnetic properties of exoplanets.

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