<< Cosmo.ToK %TOC% ---- ---+ ToK Warszawa meeting - Rough Notes Sun 18 Feb 2007 %RED% *These are just rough notes - feel free to correct them, add links, etc.* %ENDCOLOR% ---++ David Langlois exact non-linear approach to perturbations (continued) - ToK070216RoughNotes#Langlois_Non_linear_cosmological ---++ Mukhanov - polarisation tensor approach vs Stokes parameters polarisation tensors - vectors on sphere - %$P_{ab}$% - see also WikipediaEn:Polarization eigenvalue problem %$ P_b^a - \lambda p_b$%, %$\lambda > 0$% follow this through recombination - WikipediaEn:Thomson_scattering - requires recombination duration to be %$ >0 $%, otherwise no polarisation requires quadrupole (at least anisotropy), so from beginning of recombination epoch horizon scale at time of recombination %$ P \propto \frac{\delta T}{T} \sigma^2 \propto 10^{-2} \frac{\delta T}{T} $% B=0 for scalar polarisation from gravitational waves BB correlation %$\ll$% C_l (unpolarised)
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18 Feb 2007,
BoudRoukema
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