Simulation of this process can be facilitated with the "on-the-spot" approximation for the local diffuse field. A general solution for the dispersion function in this process is the so-called H-function developed by Chandrasekhar. Angle cosines of plus and minus one over root 3 are commonly used in the two-stream approximation for this process, which can be extended to the Eddington approximation of near-isotropy at large depth. Its grey approximation assumes a frequency-independent opacity, and its fundamental equation sets the source function minues the intensity equal to the derivative of the intensity with respect
Simulation of this process can be facilitated with the "on-the-spot" approximation for the local diffuse field. A general solution for the dispersion function in this process is the so-called H-function developed by Chandrasekhar. Angle cosines of plus and minus one over root 3 are commonly used in the two-stream approximation for this process, which can be extended to the Eddington approximation of near-isotropy at large depth. Its grey approximation assumes a frequency-independent opacity, and its fundamental equation sets the source function minues the intensity equal to the derivative of the intensity with respect to the optical depth. It occurs in a diffusive fashion as the dominant energy transport mechanism in non-convective regions of stars. For 10 points, name this process of absorption and emission into a beam of light passing through a medium.
Simulation of this process can be facilitated with the "on-the-spot" approximation for the local diffuse field.
radiative transfer