The radiative transfer for polarized radiation at second order in cosmological perturbations
arXiv:0809.3245 · doi:10.1007/s10714-009-0782-1
Abstract
This article investigates the full Boltzmann equation up to second order in the cosmological perturbations. Describing the distribution of polarized radiation by using a tensor valued distribution function, the second order Boltzmann equation, including polarization, is derived without relying on the Stokes parameters.
4 pages, no figure; replaced to match published version