Radiative transfer (also called radiation transport) is the physical phenomenon of energy transfer in the form of electromagnetic radiation. The propagation of radiation through a medium is affected by absorption, emission, and scattering processes. The equation of radiative transfer describes these interactions mathematically. Equations of radiative transfer have application in a wide variety of subjects including optics, astrophysics, atmospheric science, and remote sensing. Analytic solutions to the radiative transfer equation (RTE) exist for simple cases but for more realistic media, with complex multiple scattering effects, numerical methods are required. The present article is largely focused on the condition of radiative equilibrium.^[1][2]

Definitions

The fundamental quantity that describes a field of radiation is called spectral radiance in radiometric terms (in other fields it is often called specific intensity). For a very small area element in the radiation field, there can be electromagnetic radiation passing in both senses in every spatial direction through it. In radiometric terms, the passage can be completely characterized by the amount of energy radiated in each of the two senses in each spatial direction, per unit time, per unit area of surface of sourcing passage, per unit solid angle of reception at a distance, per unit wavelength interval being considered (polarization will be ignored for the moment).

In terms of the spectral radiance, ${\displaystyle I_{\nu }}$, the energy flowing across an area element of area ${\displaystyle da\,}$ located at ${\displaystyle \mathbf {r} }$ in time ${\displaystyle dt\,}$ in the solid angle ${\displaystyle d\Omega }$ about the direction ${\displaystyle {\hat {\mathbf {n} }}}$ in the frequency interval ${\displaystyle \nu \,}$ to ${\displaystyle \nu +d\nu \,}$ is

${\displaystyle dE_{\nu }=I_{\nu }(\mathbf {r} ,{\hat {\mathbf {n} }},t)\cos \theta \ d\nu \,da\,d\Omega \,dt}$

where ${\displaystyle \theta }$ is the angle that the unit direction vector ${\displaystyle {\hat {\mathbf {n} }}}$ makes with a normal to the area element. The units of the spectral radiance are seen to be energy/time/area/solid angle/frequency. In MKS units this would be W·m⁻²·sr⁻¹·Hz⁻¹ (watts per square-metre-steradian-hertz).

The equation of radiative transfer

The equation of radiative transfer simply says that as a beam of radiation travels, it loses energy to absorption, gains energy by emission processes, and redistributes energy by scattering. The differential form of the equation for radiative transfer is:

${\displaystyle {\frac {1}{c}}{\frac {\partial }{\partial t}}I_{\nu }+{\hat {\Omega }}\cdot \nabla I_{\nu }+(k_{\nu ,s}+k_{\nu ,a})\rho I_{\nu }=j_{\nu }\rho +{\frac {1}{4\pi }}k_{\nu ,s}\rho \int _{\Omega }I_{\nu }d\Omega }$

where ${\displaystyle c}$ is the speed of light, ${\displaystyle j_{\nu }}$ is the emission coefficient, ${\displaystyle k_{\nu ,s}}$ is the scattering opacity, ${\displaystyle k_{\nu ,a}}$ is the absorption opacity, ${\displaystyle \rho }$ is the mass density and the ${\displaystyle {\frac {1}{4\pi }}k_{\nu ,s}\int _{\Omega }I_{\nu }d\Omega }$ term represents radiation scattered from other directions onto a surface.

Solutions to the equation of radiative transfer

Solutions to the equation of radiative transfer form an enormous body of work. The differences however, are essentially due to the various forms for the emission and absorption coefficients. If scattering is ignored, then a general steady state solution in terms of the emission and absorption coefficients may be written:

${\displaystyle I_{\nu }(s)=I_{\nu }(s_{0})e^{-\tau _{\nu }(s_{0},s)}+\int _{s_{0}}^{s}j_{\nu }(s')e^{-\tau _{\nu }(s',s)}\,ds'}$

where ${\displaystyle \tau _{\nu }(s_{1},s_{2})}$ is the optical depth of the medium between positions ${\displaystyle s_{1}}$ and ${\displaystyle s_{2}}$:

${\displaystyle \tau _{\nu }(s_{1},s_{2})\ {\stackrel {\mathrm {def} }{=}}\ \int _{s_{1}}^{s_{2}}\alpha _{\nu }(s)\,ds}$

Local thermodynamic equilibrium

A particularly useful simplification of the equation of radiative transfer occurs under the conditions of local thermodynamic equilibrium (LTE). It is important to note that local equilibrium may apply only to a certain subset of particles in the system. For example, LTE is usually applied only to massive particles. In a radiating gas, the photons being emitted and absorbed by the gas do not need to be in a thermodynamic equilibrium with each other or with the massive particles of the gas in order for LTE to exist.

In this situation, the absorbing/emitting medium consists of massive particles which are locally in equilibrium with each other, and therefore have a definable temperature (Zeroth Law of Thermodynamics). The radiation field is not, however in equilibrium and is being entirely driven by the presence of the massive particles. For a medium in LTE, the emission coefficient and absorption coefficient are functions of temperature and density only, and are related by:

${\displaystyle {\frac {j_{\nu }}{\alpha _{\nu }}}=B_{\nu }(T)}$

where ${\displaystyle B_{\nu }(T)}$ is the black body spectral radiance at temperature T. The solution to the equation of radiative transfer is then:

${\displaystyle I_{\mathrm{\nu <!--\; \nu \; -->}}(s)=I_{\mathrm{\nu <!--\; \nu \; -->}}(s_0)e^{-<!--\; -\; -->{\mathrm{\tau <!--\; \tau \; -->}}_{\mathrm{\nu <!--\; \nu \; -->}}(s_0,s)}+{}_{}^{}}$Zdroj:https://en.wikipedia.org?pojem=Radiative_transfer
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