Stefan–Boltzmann law
E32546
The Stefan–Boltzmann law is a fundamental principle of thermal radiation stating that the total energy radiated per unit surface area of a black body is proportional to the fourth power of its absolute temperature.
Statements (48)
| Predicate | Object |
|---|---|
| instanceOf |
physical law
ⓘ
radiation law ⓘ |
| appliesTo |
ideal black body
ⓘ
opaque, diffuse, gray surfaces with modified emissivity ⓘ |
| approximateValueOfStefanBoltzmannConstant | 5.670374419×10^−8 W⋅m^−2⋅K^−4 ⓘ |
| assumes | surface is a perfect black body with emissivity equal to 1 ⓘ |
| category | laws of thermodynamics and statistical mechanics ⓘ |
| dependsOn | absolute temperature in kelvins ⓘ |
| derivationYear | 1884 ⓘ |
| derivedBy | Ludwig Boltzmann ⓘ |
| derivedFrom |
Planck radiation law
ⓘ
surface form:
Planck’s law of black-body radiation
thermodynamics of electromagnetic radiation ⓘ |
| describes | total radiant heat power emitted per unit area of a black body ⓘ |
| dimensionOfStefanBoltzmannConstant | power per area per temperature to the fourth power ⓘ |
| emissivityRange | 0 to 1 ⓘ |
| field |
astrophysics
ⓘ
statistical mechanics ⓘ thermal radiation ⓘ thermodynamics ⓘ |
| generalization | radiant exitance of a real surface is M = ε σ T^4 ⓘ |
| includesParameter | emissivity ⓘ |
| isIntegralOver |
Planck spectral radiance over all wavelengths
ⓘ
all solid angles of emission ⓘ |
| mathematicalForm | j* = σ T^4 ⓘ |
| namedAfter |
Josef Stefan
ⓘ
Ludwig Boltzmann ⓘ |
| proportionalTo | fourth power of absolute temperature ⓘ |
| proposedBy | Josef Stefan ⓘ |
| relatedTo |
Kirchhoff's law of thermal radiation
ⓘ
surface form:
Kirchhoff’s law of thermal radiation
Planck radiation law ⓘ
surface form:
Planck’s law
Wien displacement law ⓘ
surface form:
Wien’s displacement law
black-body radiation ⓘ |
| SIUnitOfStefanBoltzmannConstant | watt per square metre per kelvin to the fourth power ⓘ |
| states | the total energy radiated per unit surface area of a black body is proportional to the fourth power of its absolute temperature ⓘ |
| symbolOfRadiantExitance | j* ⓘ |
| symbolOfStefanBoltzmannConstant | σ ⓘ |
| symbolOfTemperature | T ⓘ |
| usedFor |
calculating radiative heat transfer
ⓘ
climate modeling ⓘ estimating luminosity of stars ⓘ relating stellar radius, temperature and luminosity ⓘ thermal engineering ⓘ |
| usedIn |
design of furnaces and radiative heaters
ⓘ
planetary energy balance models ⓘ radiative heat transfer calculations between surfaces ⓘ remote sensing of surface temperatures ⓘ |
| validFor | thermal equilibrium ⓘ |
| yearProposed | 1879 ⓘ |
Referenced by (6)
Full triples — surface form annotated when it differs from this entity's canonical label.