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  2. Planetary equilibrium temperature - Wikipedia

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

    Planetary equilibrium temperature differs from the global mean temperature and surface air temperature, which are measured observationally by satellites or surface-based instruments, and may be warmer than the equilibrium temperature due to the greenhouse effect.

  3. 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 ...

  4. Kepler-42 - Wikipedia

    en.wikipedia.org/wiki/Kepler-42

    Based on the orbits of the planets and the luminosity and effective temperature of the host star, the equilibrium temperatures of the planets can be calculated. Assuming an extremely high albedo of 0.9 and absence of greenhouse effect , the outer planet Kepler-42 d would have an equilibrium temperature of about 280 K (7 °C), [ 7 ] similar to ...

  5. 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.

  6. 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 ...

  7. 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]

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  9. 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.