This tool is employed to compute either the peak wavelength of electromagnetic radiation emitted by a black body or the temperature of the black body itself. The calculation relies on the direct relationship between these two variables, as described by a fundamental physical principle. For example, if the temperature of an object is known, the instrument determines the wavelength at which the emitted radiation is most intense. Conversely, if the peak emission wavelength is observed, the temperature of the radiating body can be derived.
The significance of this computational aid lies in its ability to provide insights into the thermal characteristics of distant objects, such as stars, without direct physical contact. In astrophysics, it allows for the determination of stellar surface temperatures based on observed spectra. Historically, the underlying principle played a crucial role in the development of quantum mechanics by highlighting the limitations of classical physics in explaining black body radiation.
