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  2. Earth's internal heat budget - Wikipedia

    en.wikipedia.org/wiki/Earth's_internal_heat_budget

    Primordial heat is the heat lost by the Earth as it continues to cool from its original formation, and this is in contrast to its still actively-produced radiogenic heat. The Earth core's heat flow—heat leaving the core and flowing into the overlying mantle—is thought to be due to primordial heat, and is estimated at 5–15 TW. [23]

  3. Gravitational compression - Wikipedia

    en.wikipedia.org/wiki/Gravitational_compression

    At the center of a planet or star, gravitational compression produces heat by the Kelvin–Helmholtz mechanism. This is the mechanism that explains how Jupiter continues to radiate heat produced by its gravitational compression. [1] The most common reference to gravitational compression is stellar evolution.

  4. Internal heating - Wikipedia

    en.wikipedia.org/wiki/Internal_heating

    Internal heat is the heat source from the interior of celestial objects, such as stars, brown dwarfs, planets, moons, dwarf planets, and (in the early history of the Solar System) even asteroids such as Vesta, resulting from contraction caused by gravity (the Kelvin–Helmholtz mechanism), nuclear fusion, tidal heating, core solidification (heat of fusion released as molten core material ...

  5. Omegaverse - Wikipedia

    en.wikipedia.org/wiki/Omegaverse

    The Omegaverse exploded in popularity in 2017, quickly becoming a frequent subject of fan fiction writers. [29] As of July 2018, over 39,000 Omegaverse fan works had been published on the fan fiction website Archive of Our Own, [9] and over 165,000 as of 2023. [39]

  6. Radiative equilibrium - Wikipedia

    en.wikipedia.org/wiki/Radiative_equilibrium

    Liou (2002, page 459) [16] and other authors use the term global radiative equilibrium to refer to radiative exchange equilibrium globally between Earth and extraterrestrial space; such authors intend to mean that, in the theoretical, incoming solar radiation absorbed by Earth's surface and its atmosphere would be equal to outgoing longwave ...

  7. Thermal history of Earth - Wikipedia

    en.wikipedia.org/wiki/Thermal_history_of_Earth

    In 1862, Lord Kelvin calculated the age of the Earth at between 20 million and 400 million years by assuming that Earth had formed as a completely molten object, and determined the amount of time it would take for the near-surface to cool to its present temperature. Since uniformitarianism required a much older Earth, there was a contradiction.

  8. Planetary equilibrium temperature - Wikipedia

    en.wikipedia.org/wiki/Planetary_equilibrium...

    There are large variations in surface temperature over space and time on airless or near-airless bodies like Mars, which has daily surface temperature variations of 50–60 K. [18] [19] Because of a relative lack of air to transport or retain heat, significant variations in temperature develop. Assuming the planet radiates as a blackbody (i.e ...

  9. Earth's energy budget - Wikipedia

    en.wikipedia.org/wiki/Earth's_energy_budget

    The geothermal heat flow from the Earth's interior is estimated to be 47 terawatts (TW) [12] and split approximately equally between radiogenic heat and heat left over from the Earth's formation. This corresponds to an average flux of 0.087 W/m 2 and represents only 0.027% of Earth's total energy budget at the surface, being dwarfed by the 173 ...