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Table 4

Kinetic power from the night side of the exoplanet for different IMF orientations (B6000 model).

[P(DS)] (105 W)
Model Bx Bxneg By Byneg Bz Bzneg
B250 0.63 0.63 6.90 8.72 5.96 11.3
B1000 2.18 2.04 12.4 12.2 10.6 29.5
B6000 4.34 4.21 35.0 32.5 14.7 72.5

Linear regression slope day side vs. Bex (1011 W/T)
             
Bx Bxneg By Byneg Bz Bzneg

α 0.77 0.74 6.05 5.65 2.71 12.6
Δ α ± 0.1 ± 0.1 ± 1 ± 1 ± 1 ± 2

[P(NS)] (105 W)
             
Model Bx Bxneg By Byneg Bz Bzneg

B250 0.10 0.10 0.53 0.53 0.13 0.18
B1000 1.04 0.72 1.74 1.71 1.00 0.66
B6000 10.2 10.2 15.8 16.4 7.75 20.4

Linear regression slope night side (1011 W/T)
             
Bx Bxneg By Byneg Bz Bzneg

α 1.68 1.67 2.61 2.70 1.28 3.32
Δ α ± 0.08 ± 0.1 ± 0.1 ± 0.1 ± 0.04 ± 0.3

Notes. Expected radio emission on the exoplanet’s day side (first table) and in the magnetotail X point on the exoplanet’s night side (third table) for different IMF orientations (a = 0, b = 2 ×10−3) and exoplanet magnetic field intensities. Slope (α) and goodness of fit (Δα) of the linear regression [P] = αBex for each IMF orientation (second and fourth table). Bex is the magnetic field intensity on the exoplanet surface and the exoplanet radius is Rex = 2440 km.

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