Svartelegemefordelinger

Svartelegemefordelinger, in a Norwegian-language context, refers to the spectral energy distributions of idealized black bodies, describing how radiative power is distributed across wavelengths or frequencies for a given temperature. As a concept, blackbody distributions are the reference standard for thermal radiation and are used to model the emission of any object when its emissivity is close to unity.

The distributions are governed by Planck’s law. The spectral radiance can be expressed in two common forms: Bν(T) = (2hν^3/c^2) / (exp(hν/kT) − 1) per unit frequency, or Bλ(T) = (2hc^2/λ^5) / (exp(hc/(λkT)) − 1) per unit wavelength. These forms describe how a black body at temperature T emits energy at different frequencies ν or wavelengths λ. Integrating over all frequencies yields the total emitted power per unit area, M(T) = σT^4, where σ is the Stefan-Boltzmann constant (approximately 5.6704 × 10^−8 W/m^2K^4). Wien’s displacement law, λmax T = b (with b ≈ 2.8978 × 10^−3 m·K), gives the wavelength at which emission peaks for a given temperature.

Real-world objects often deviate from an ideal black body due to emissivity ε(λ) < 1 and spectral variation. The concept of svartelegemefordelinger thus underpins radiometry, thermography, stellar astrophysics, and climate science, providing a baseline against which actual spectra are compared and interpreted. The framework originated with Planck’s quantum hypothesis at the turn of the 20th century and remains central to modern physics and engineering.