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  2. Planetary equilibrium temperature - Wikipedia

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

    On airless bodies, the lack of any significant greenhouse effect allows equilibrium temperatures to approach mean surface temperatures, as on Mars, [5] where the equilibrium temperature is 210 K (−63 °C; −82 °F) and the mean surface temperature of emission is 215 K (−58 °C; −73 °F). [6]

  3. LHS 1140 b - Wikipedia

    en.wikipedia.org/wiki/LHS_1140_b

    LHS 1140 b orbits close to the outer edge of the habitable zone, a region around a star where temperatures are just right for liquid water to pool on the surface of orbiting planets, given sufficient atmospheric pressure. [7] The equilibrium temperature of LHS 1140 b is rather low, at 230 K (−43 °C; −46 °F), as cold as the polar regions ...

  4. Runaway greenhouse effect - Wikipedia

    en.wikipedia.org/wiki/Runaway_greenhouse_effect

    The runaway greenhouse effect is often formulated in terms of how the surface temperature of a planet changes with differing amounts of received starlight. [13] If the planet is assumed to be in radiative equilibrium, then the runaway greenhouse state is calculated as the equilibrium state at which water cannot exist in liquid form. [3]

  5. Idealized greenhouse model - Wikipedia

    en.wikipedia.org/wiki/Idealized_greenhouse_model

    The temperatures of a planet's surface and atmosphere are governed by a delicate balancing of their energy flows. The idealized greenhouse model is based on the fact that certain gases in the Earth's atmosphere , including carbon dioxide and water vapour , are transparent to the high-frequency solar radiation , but are much more opaque to the ...

  6. Atmospheric thermodynamics - Wikipedia

    en.wikipedia.org/wiki/Atmospheric_thermodynamics

    Atmospheric thermodynamics is the study of heat-to-work transformations (and their reverse) that take place in the Earth's atmosphere and manifest as weather or climate. . Atmospheric thermodynamics use the laws of classical thermodynamics, to describe and explain such phenomena as the properties of moist air, the formation of clouds, atmospheric convection, boundary layer meteorology, and ...

  7. TRAPPIST-1f - Wikipedia

    en.wikipedia.org/wiki/TRAPPIST-1f

    Simulations in 2017 suggested the planet is approximately 20% water by composition, much higher than that of Earth. With such a massive water envelope, the pressure and temperature will be high enough to keep the water in a gaseous state and any liquid water will only exist as clouds near the top of TRAPPIST-1f's atmosphere.

  8. Triple point of water - Wikipedia

    en.wikipedia.org/wiki/Triple_point

    A typical phase diagram.The solid green line applies to most substances; the dashed green line gives the anomalous behavior of water. In thermodynamics, the triple point of a substance is the temperature and pressure at which the three phases (gas, liquid, and solid) of that substance coexist in thermodynamic equilibrium. [1]

  9. Water (data page) - Wikipedia

    en.wikipedia.org/wiki/Water_(data_page)

    Data in the table above is given for water–steam equilibria at various temperatures over the entire temperature range at which liquid water can exist. Pressure of the equilibrium is given in the second column in kPa. The third column is the heat content of each gram of the liquid phase relative to water at 0 °C.

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