Photon diffusion

In astrophysics, photon diffusion occurs inside a stellar atmosphere. To describe this phenomenon, one should develop the transfer equation in moments and use the Eddington approximation to radiative transfer (i.e. the diffusion approximation). In 3D the results are two equations for the photon energy flux:

${\displaystyle {\vec {F}}=-{\frac {c}{12\pi \sigma }}{\vec {\nabla }}U,}$

${\displaystyle {\vec {\nabla }}\cdot {\vec {F}}=0,}$

where ${\displaystyle \sigma }$ is the opacity. By substituting the first equation into the second, one obtains the diffusion equation for the photon energy density:

${\displaystyle \nabla ^{2}U-{\frac {1}{\sigma }}{\vec {\nabla }}U\cdot {\vec {\nabla }}\sigma =0.}$

In medicine, the diffusion of photons can be used to create images of the body (mainly brain and breast) and has contributed much to the advance of certain fields of research, such as neuroscience. This technique is known as diffuse optical imaging.

• Diffuse reflection
• Diffusion damping
• Global dimming
• Medical optical imaging
• Optical tomography
• Radiative transfer equation and diffusion theory for photon transport in biological tissue