Thermal structure of Jupiter

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Abstract
The observed net flux of energy from the surface of Jupiter is assumed to derive from the thermal energy of the protons in the interior of the planet The thermodynamics and transport properties of metallic hydrogen at finite temperature are discussed, and the temperature distribution in the interior is calculated for various assumed luminosities and atmospheric boundary conditions. The resulting mod- els possess deep convective envelopes for surface fluxes in excess of _.~,1O2 ergs cm~ sec' and are wholly convective for surface fluxes exceeding ~-~-`1O~ ergs cm~ sec'

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