Linked from

The 27 pages that link to Stefan–Boltzmann law, each with the reason it gives.

• Heat transferBroader topic: It quantifies radiative heat transfer from hot surfaces.

• Thermal radiationRelated: It connects total emitted power to temperature.

• Black-body radiationRelated: Integrating the spectrum yields this temperature dependence of total emitted power.

• Planck's lawBroader topic: Integrating Planck's spectrum over all wavelengths yields this total-power relation.

• Earth's energy budgetRelated: It links Earth's temperature to the strength of its thermal emissions.

• Stellar luminosityRelated: It relates a star’s effective temperature and radius to its total luminosity.

• EmissivityRelated: For a gray surface, total emission is commonly expressed as emissivity times black-body emission.

• Stellar radiusRelated: Together with luminosity and effective temperature, it yields a star’s radius.

• Yarkovsky effectRelated: It describes how strongly hotter surface regions contribute to thermal recoil.

• Kirchhoff's law of thermal radiationCompared with: It governs total emitted power rather than matching emissivity to absorptivity by mode.

• Rayleigh–Jeans lawRelated: Unlike the frequency-resolved Rayleigh–Jeans law, it gives total emission integrated over the spectrum.

• Infrared thermographyRelated: It relates total thermal emission to temperature, though cameras usually analyze spectral bands.

• Radiative coolingRelated: It quantifies how strongly thermal emission rises as a surface warms.

• Wien's displacement lawRelated: It describes total emission, complementing this law’s description of where emission peaks.

• Fourier's lawCompared with: It governs radiative transfer, which does not require the conductive temperature-gradient relation.

• Solar luminosityRelated: Applied to the Sun’s radius and effective temperature, it yields its radiated power.

• Absolute temperatureRelated: The fourth-power dependence makes absolute temperature essential to thermal-radiation calculations.

• Planetary equilibrium temperatureRelated: It converts a planet’s outgoing thermal radiation into the temperature required for energy balance.

• Bolometric luminosityRelated: Combined with stellar radius, it relates surface temperature to total luminosity.

• Newton's law of coolingCompared with: Radiative cooling is nonlinear in temperature, unlike the law's linear temperature-difference assumption.

• Radiative equilibriumRelated: It relates a body’s temperature to its thermal emission in a simple equilibrium calculation.

• Wilhelm WienRelated: It complements Wien’s law by relating temperature to total emitted radiation rather than peak wavelength.

• Black bodyRelated: It gives the total energy emitted across the black body's spectrum.

• Photon gasRelated: It describes how the photon gas’s energy density rises sharply with temperature.

• Outgoing longwave radiationRelated: It links the temperatures of emitting surfaces and atmospheric layers to their infrared emission.

• Stefan–Boltzmann constantRelated: This law gives the constant its defining place in thermal radiation.

• UY ScutiRelated: It links measured luminosity and temperature to inferred stellar radius.