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Fig. 2


Energy flux at the top of the atmosphere of a 0.5 Earth-mass moon orbiting a 5 Jupiter-mass planet at 1 AU distance from a Sun-like star; tidal heating is calculated with a viscoelastic model. The same colours, contours and signatures were applied as in Fig. 1. Note that the viscoelastic model is valid only for small orbital eccentricities. Heating contours in the upper half of the panel (above 0.1 along the ordinate) could be off by orders of magnitude in real cases.

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