Radiance of black body from temperature¶
The Stefan—Boltzmann law, also known as Stefan’s law, states that the total energy radiated per unit surface area of a black body per unit time is directly proportional to the fourth power of the black body’s thermodynamic temperature.
Notation:
\(\sigma\) (
sigma) isstefan_boltzmann_constant.
Conditions:
The body is completely black, i.e. it absorbs all energy.
Links:
- radiance¶
radiant_exitanceof the body.
- Symbol:
M_e- Latex:
\(M_\text{e}\)
- Dimension:
power/area
- temperature¶
temperatureof the body.
- Symbol:
T- Latex:
\(T\)
- Dimension:
temperature
- law¶
M_e = sigma * T^4- Latex:
- \[M_\text{e} = \sigma T^{4}\]