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:**

#. :math:`\sigma` (:code:`sigma`) is :attr:`~symplyphysics.quantities.stefan_boltzmann_constant`.

**Conditions:**

#. The body is completely black, i.e. it absorbs all energy.

**Links:**

#. `Wikipedia <https://en.wikipedia.org/wiki/Stefan%E2%80%93Boltzmann_law>`__.

.. py:currentmodule:: symplyphysics.laws.thermodynamics.radiance_of_black_body_from_temperature

.. py:data:: radiance

    :attr:`~symplyphysics.symbols.optics.radiant_exitance` of the body.

Symbol:
    :code:`M_e`

Latex:
    :math:`M_\text{e}`

Dimension:
    :code:`power/area`


.. py:data:: temperature

    :attr:`~symplyphysics.symbols.thermodynamics.temperature` of the body.

Symbol:
    :code:`T`

Latex:
    :math:`T`

Dimension:
    :code:`temperature`


.. py:data:: law

    :code:`M_e = sigma * T^4`


    Latex:
        .. math::
            M_\text{e} = \sigma T^{4}