Cosmic Microwave Background Anisotropies up to Second Order

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dc.creatorBartolo, Nicola
dc.creatorMatarrese, Sabino
dc.creatorRiotto, Antonio
dc.date2007-03-19
dc.date2007-04-05
dc.date.accessioned2026-07-07T07:54:35Z
dc.date.available2026-07-07T07:54:35Z
dc.descriptionThese lecture notes present the computation of the full system of Boltzmann equations describing the evolution of the photon, baryon and cold dark matter fluids up to second order in perturbation theory, as recently studied in (Bartolo, Matarrese & Riotto 2006, 2007). These equations allow to follow the time evolution of the cosmic microwave background anisotropies at all angular scales from the early epoch, when the cosmological perturbations were generated, to the present, through the recombination era. The inclusion of second-order contributions is mandatory when one is interested in studying possible deviations from Gaussianity of cosmological perturbations, either of primordial (e.g. inflationary) origin or due to their subsequent evolution. Most of the emphasis in these lectures notes will be given to the derivation of the relevant equations for the study of cosmic microwave background anisotropies and to their analytical solutions.
dc.description53 pages, LaTeX file. Lectures given by S.M. at Les Houches Summer School - Session 86: Particle Physics and Cosmology: The Fabric of Spacetime, Les Houches, France, 31 Jul - 25 Aug 2006. To appear in the Proceedings. Second version with minor misprints corrected
dc.identifierhttps://arxiv.org/abs/astro-ph/0703496
dc.identifierhttp://arxiv.org/abs/astro-ph/0703496
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/126668
dc.subjectAstrophysics
dc.subjectGeneral Relativity and Quantum Cosmology
dc.subjectHigh Energy Physics - Phenomenology
dc.titleCosmic Microwave Background Anisotropies up to Second Order
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