Fig. 11
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Temperature-pressure profiles of the envelopes of Jupiter and Saturn at different ages, for adiabatic and super-adiabatic interiors. We compare calculations shown on Fig. 10. Dash-dotted lines show T − P profiles of our baseline models, assuming adiabaticity (Rρ = 0). Solid lines show T − P profiles for Rρ = 0.1 for Jupiter (top panel) and Rρ = 0.008 for Saturn (bottom panel).
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