= Solution
For typical well-mixed structures, the dominant processes are:
* \b[<Gas giant> interiors:] efficient <convection> through most of the deep fluid envelope; <radiative transfer> releases the heat near the <photosphere>.
* \b[Rocky interiors:] slow solid-state <mantle convection> over geological time, with <heat conduction> dominant across the rigid <lithosphere>. A liquid core can also convect; being solid does not prevent creep-driven heat transport in the mantle.
* \b[Weakly irradiated giant atmospheres at $0.1$–$10\,\mathrm{bar}$:] usually <convection> in the <planetary troposphere>, becoming radiative near and above the <tropopause>. The transition pressure and cloud or compositional effects vary between planets.
* \b[Strongly irradiated <hot Jupiter> atmospheres at $0.1$–$10\,\mathrm{bar}$:] usually a stable radiative region; the deep <radiative-convective boundary> can lie at substantially larger pressure. Atmospheric winds also redistribute energy horizontally.
Representative temperatures must specify the level: \b[<Earth> has about $288\,\mathrm K$ at the surface] (about $255\,\mathrm K$ effective emission temperature); \b[<Jupiter> has about $165\,\mathrm K$ near one bar] (about $125\,\mathrm K$ effective temperature); \b[<hot Jupiters> commonly have photospheric temperatures of order $1000$–$2500\,\mathrm K$]; and \b[the <Sun>'s <photosphere> is about $5800\,\mathrm K$]. Upper layers, nightsides, deep interiors and the solar corona have different temperatures. These are characteristic values, not constant temperatures throughout each atmosphere.
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