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  2. Planetary equilibrium temperature - Wikipedia

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

    The effective radiation emission temperature is a related concept, [2] but focuses on the actual power radiated rather than on the power being received, and so may have a different value if the planet has an internal energy source or when the planet is not in radiative equilibrium. [3] [4] Planetary equilibrium temperature differs from the ...

  3. Idealized greenhouse model - Wikipedia

    en.wikipedia.org/wiki/Idealized_greenhouse_model

    [3] [4] [5] The planet is idealized by the model as being functionally "layered" with regard to a sequence of simplified energy flows, but dimensionless (i.e. a zero-dimensional model) in terms of its mathematical space. [6] The layers include a surface with constant temperature T s and an atmospheric layer with constant temperature T a. For ...

  4. Effective temperature - Wikipedia

    en.wikipedia.org/wiki/Effective_temperature

    The effective temperature of the Sun (5778 kelvins) is the temperature a black body of the same size must have to yield the same total emissive power.. The effective temperature of a star is the temperature of a black body with the same luminosity per surface area (F Bol) as the star and is defined according to the Stefan–Boltzmann law F Bol = σT eff 4.

  5. Earth's energy budget - Wikipedia

    en.wikipedia.org/wiki/Earth's_energy_budget

    The strong (fourth-power) temperature sensitivity maintains a near-balance of the outgoing energy flow to the incoming flow via small changes in the planet's absolute temperatures. Increase in the Earth's non-cloud greenhouse effect (2000–2022) based on satellite data.

  6. Komabayashi–Ingersoll limit - Wikipedia

    en.wikipedia.org/wiki/Komabayashi–Ingersoll_limit

    In planetary science, the Komabayashi–Ingersoll limit represents the maximum solar flux a planet can handle without a runaway greenhouse effect setting in. [1] [2] [3]. For planets with temperature-dependent sources of greenhouse gases such as liquid water and optically thin atmospheres the outgoing longwave radiation curve (which indicates how fast energy can be radiated away by the planet ...

  7. Greenhouse effect - Wikipedia

    en.wikipedia.org/wiki/Greenhouse_effect

    When the planet is in radiative equilibrium, the overall effective temperature of the planet is given by T e f f = T r a d e q . {\displaystyle T_{\mathrm {eff} }=T_{\mathrm {radeq} }\;.} Thus, the concept of radiative equilibrium is important because it indicates what effective temperature a planet will tend towards having.

  8. The Most Incompatible Zodiac Signs That Should Never, Ever ...

    www.aol.com/lifestyle/most-incompatible-zodiac...

    At its most basic level, my understanding from talking with Wright is that zodiac sign incompatibility typically arises from differences in elements (fire, earth, air, and water) and the signs ...

  9. Radiative forcing - Wikipedia

    en.wikipedia.org/wiki/Radiative_forcing

    Radiative forcing is defined in the IPCC Sixth Assessment Report as follows: "The change in the net, downward minus upward, radiative flux (expressed in W/m 2) due to a change in an external driver of climate change, such as a change in the concentration of carbon dioxide (CO 2), the concentration of volcanic aerosols or the output of the Sun." [3]: 2245