Wien's Displacement Law provides a critical insight into understanding the behavior of blackbody radiation in terms of temperature and wavelength. This law states that the peak wavelength of the emitted radiation from a blackbody is inversely proportional to its temperature. The formula for Wien's Displacement Law is:
where:
- is the peak wavelength,
- is Wien's displacement constant, approximately , and
- is the temperature in Kelvin.
In essence, as the temperature of a blackbody increases, the wavelength at which it emits most prominently shifts toward shorter wavelengths. Hence, hotter stars will have peak emissions in shorter wavelengths, meaning they appear bluer. Conversely, cooler stars will peak at longer wavelengths, often displaying a reddish color. This principle helps astronomers determine stellar temperatures based on their color.