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Stefan–Boltzmann Law

The Stefan–Boltzmann law describes the power radiated from a blackbody in terms of its temperature. Specifically, the Stefan–Boltzmann law states that the total energy radiated per unit surface area of a blackbody across all wavelengths per unit time (also known as the blackbody radiant emittance or radiant exitance) is directly proportional to the fourth power of the blackbody's thermodynamic temperature.

The radiant exitance equals the product of the Stefan-Boltzmann constant, emissivity and the temperature to the fourth power.

Formula

QuantityVariable["M", "RadiantExitance"] == Quantity[1, "StefanBoltzmannConstant"]*QuantityVariable["T", "Temperature"]^4*QuantityVariable["ε", "Emissivity"]

symbol description physical quantity
M radiant exitance "RadiantExitance"
T temperature "Temperature"
ε emissivity "Emissivity"

Forms

Examples

Get the resource:

In[1]:=
ResourceObject["Stefan\[Dash]Boltzmann Law"]
Out[1]=

Get the formula:

In[2]:=
FormulaData[ResourceObject["Stefan\[Dash]Boltzmann Law"]]
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Use some values:

In[3]:=
FormulaData[ ResourceObject[ "Stefan\[Dash]Boltzmann Law"], {QuantityVariable[ "T","Temperature"] -> Quantity[310, "Kelvins"], QuantityVariable["M","RadiantExitance"] -> Quantity[1, ("Watts")/("Meters")^2]}]
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Source Metadata

  • Creator:
  • Date: 1879

Publisher Information