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.
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Pitrou, C. The radiative transfer for polarized radiation at second order in cosmological perturbations. Gen Relativ Gravit 41, 2587–2595 (2009). https://doi.org/10.1007/s10714-009-0782-1
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DOI: https://doi.org/10.1007/s10714-009-0782-1