Linked from

The 95 pages that link to Black-body radiation, each with the reason it gives.

• Color temperatureNarrower topic: Its spectrum shifts toward shorter wavelengths as the blackbody heats, creating the temperature-to-color relationship.

• Planck's lawNarrower topic: Planck's law specifies the spectrum of this idealized thermal radiation.

• Hertzsprung–Russell diagramNarrower topic: It explains why stellar color and spectral shape reveal surface temperature.

• Stefan–Boltzmann lawNarrower topic: The law summarizes the total emitted power across this spectrum.

• Earth's energy budgetNarrower topic: It supplies a useful baseline for understanding planetary heat emission.

• Ultraviolet catastropheNarrower topic: The catastrophe is a failed classical prediction about this radiation’s spectrum.

• Rayleigh–Jeans lawNarrower topic: The law is a classical prediction for the spectrum of this thermal radiation.

• Infrared thermographyNarrower topic: It provides the physical reference for relating emitted infrared radiation to temperature.

• Wien's displacement lawNarrower topic: The law describes how this spectrum’s peak wavelength changes as the blackbody’s temperature changes.

• Correlated color temperatureNarrower topic: CCT borrows its temperature scale from this thermal phenomenon, although many light sources do not emit such spectra.

• Wien approximationNarrower topic: The approximation arose in attempts to describe this thermal spectrum.

• Wilhelm WienNarrower topic: Wien’s laws describe how this radiation varies with wavelength and temperature.

• Planckian locusNarrower topic: The ideal radiator is the physical reference, not a description of every source near the curve.

• Stefan–Boltzmann constantNarrower topic: The constant summarizes the total power across this full radiation spectrum.