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  2. 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.

  3. Planetary equilibrium temperature - Wikipedia

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

    Other authors use different names for this concept, such as equivalent blackbody temperature of a planet. [1] 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 ...

  4. Black-body radiation - Wikipedia

    en.wikipedia.org/wiki/Black-body_radiation

    The blackbody law may be used to estimate the temperature of a planet orbiting the Sun. Earth's longwave thermal radiation intensity, from clouds, atmosphere and ground. The temperature of a planet depends on several factors: Incident radiation from its star; Emitted radiation of the planet (for example, Earth's infrared glow)

  5. Emissivity - Wikipedia

    en.wikipedia.org/wiki/Emissivity

    At a lower limit, clear sky (cloud-free) conditions promote the largest opening of transmission windows. The more uniform concentration of long-lived trace greenhouse gases in combination with water vapor pressures of 0.25-20 mbar then yield minimum values in the range of ε a =0.55-0.8 (with ε=0.35-0.75 for a simulated water-vapor-only ...

  6. Betelgeuse - Wikipedia

    en.wikipedia.org/wiki/Betelgeuse

    Uncertainty in the star's surface temperature, diameter, and distance make it difficult to achieve a precise measurement of Betelgeuse's luminosity, but research from 2012 quotes a luminosity of around 126,000 L ☉, assuming a distance of 200 pc. [142] Studies since 2001 report effective temperatures ranging from 3,250 to 3,690 K.

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  8. Stefan–Boltzmann law - Wikipedia

    en.wikipedia.org/wiki/Stefan–Boltzmann_law

    The temperature Stefan obtained was a median value of previous ones, 1950 °C and the absolute thermodynamic one 2200 K. As 2.57 4 = 43.5, it follows from the law that the temperature of the Sun is 2.57 times greater than the temperature of the lamella, so Stefan got a value of 5430 °C or 5700 K. This was the first sensible value for the ...

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