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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 ...
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.
Emissivity of a body at a given temperature is the ratio of the total emissive power of a body to the total emissive power of a perfectly black body at that temperature. Following Planck's law , the total energy radiated increases with temperature while the peak of the emission spectrum shifts to shorter wavelengths.
The Sun closely approximates a black-body radiator. The effective temperature, defined by the total radiative power per square unit, is 5772 K. [12] The color temperature of sunlight above the atmosphere is about 5900 K. [13] The Sun may appear red, orange, yellow, or white from Earth, depending on its position in the sky.
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A black body radiator used in CARLO laboratory in Poland. It is an approximation of a model described by Planck's law utilized as a spectral irradiance standard.. As the temperature of a black body decreases, its radiation intensity also decreases and its peak moves to longer wavelengths.
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