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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.
These particles form a part of the black body spectrum, in addition to the electromagnetic radiation. [52] A black body at room temperature (23 °C (296 K; 73 °F)) radiates mostly in the infrared spectrum, which cannot be perceived by the human eye, [53] but can be sensed by some reptiles. As the object increases in temperature to about 500 ...
The temperature of stars other than the Sun can be approximated using a similar means by treating the emitted energy as a black body radiation. [27] So: = where L is the luminosity, σ is the Stefan–Boltzmann constant, R is the stellar radius and T is the effective temperature.
A black body or blackbody is an idealized physical body that absorbs all incident electromagnetic radiation, regardless of frequency or angle of incidence. The radiation emitted by a black body in thermal equilibrium with its environment is called black-body radiation. The name "black body" is given because it absorbs all colors of light.
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The surface of a perfect black body (with an emissivity of 1) emits thermal radiation at the rate of approximately 448 watts per square metre (W/m 2) at a room temperature of 25 °C (298 K; 77 °F). Objects have emissivities less than 1.0, and emit radiation at correspondingly lower rates.
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