Calculate the total power emitted and the peak wavelength of radiation from a blackbody at a given temperature.
Source Parameters
m²
Radiation Output
Enter parameters to calculate
About this calculator
Quick Reference
σStefan-Boltzmann constant (5.67e-8)
εEmissivity (0.0 to 1.0)
ASurface area in m²
TAbsolute temperature in Kelvin
Overview
A blackbody is an idealized physical body that absorbs all incident electromagnetic radiation. The Stefan-Boltzmann law describes the power radiated from a blackbody in terms of its temperature.
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Pro Tips
The total power radiated is proportional to the fourth power of the absolute temperature (T⁴).
Wien's displacement law relates temperature to the peak wavelength of the emitted spectrum.
Ideal blackbodies have an emissivity (ε) of 1.0.
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Fun Facts
"The Sun emits radiation almost like a blackbody with a temperature of about 5,778 K."
"The peak wavelength of the Sun's radiation is in the visible green spectrum (~500 nm)."
"Wien's law is how astronomers determine the temperature of distant stars."
