Convective mixing in distant and close-in giant planets - Dependences on the initial composition, luminosity, bloating, and semi-convection

Open Access

Fig. 1

Total luminosity (blue), bloating luminosity (orange), and intrinsic luminosity (green) as a function of pressure for a planet at 0.03 AU. The intrinsic luminosity scales as $\frac{d l}{d m} = \frac{L}{M}$ $\[\frac{\mathrm{d} l}{\mathrm{~d} m}=\frac{L}{M}\]$ , and the bloating luminosity follows a power law, L ∝ P^−0.6, between 10³ and 10⁶ bar.

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