Table 3
Tidal heat flux (in W/m2) for all T 1 planets.
| Planet | Minimum eccentricity | Maximum eccentricity | ||
|---|---|---|---|---|
| Smallest core | Biggest core | Smallest core | Biggest core | |
| T-1b | ![]() |
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| T-1c | ![]() |
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| T-1d | ![]() |
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| T-1e | ![]() |
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| T-1f | ![]() |
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| T-1g | ![]() |
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| T-1h | ![]() |
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Notes. Computations were done for α=0.25 and reference temperatures (670 K for b and c, 650 K for d, 300 K for e, 250 K for f, 210 K for g, and 170 K for h). The uncertainties show the impact of α and the temperature (viscosity) profile with the lower flux values corresponding to α=0.30 and the lowest temperatures and the higher flux values corresponding to α=0.20 and the highest temperatures. For comparison, the heat flux of Io is 2.54 W/m2, the heat flux of the Earth is 8.7 e-2 W/m2, and the tidal heat flux of the Earth is 2.23 e-4 W/m2. Values in gray identify where the flux is lower than the flux of the Earth, and values in dark red are higher than the flux of Io.
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