Massive neutrinos and the anisotropy of the cosmic microwave background radiation

Details Massive neutrinos and the anisotropy of the cosmic microwave background radiation Massive neutrinos and the anisotropy of the cosmic microwave background radiation

Oct 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983mnras.205...91s&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 205, Oct. 1983, p. 91-104. Research supported by the Po

Physics

4

Background Radiation, Cosmic Noise, Microwave Emission, Neutrinos, Relic Radiation, Anisotropy, Autocorrelation, Field Theory (Physics), Mass Distribution, Perturbation

Scientific paper

The evolution of primeval adiabatic perturbations in a universe dominated by massive neutrinos is considered, and an estimate is made of the relic radiation in such a model. The approach is similar to that taken by Peebles (1982), although the integration method is different. The treatment of the gravitational instability serves as the basis for the calculation of the relic radiation anisotropy. The computations start shortly after the decoupling of neutrinos from the rest of the matter. It is noted that the perturbations in both components are related as a consequence of their previous contact. Since the approach is linear, the perturbations are decomposed into plane waves; simple power-law spectra are assumed for the initial amplitudes. The evolution of each wavelength is followed separately, and the final spectra are computed. The autocorrelation function for the mass distribution is also obtained, and its comparison with the measured galaxy autocorrelation function seerves as a normalization condition. It is noted that this normalization defines the strength of plasma perturbations at the recombination epoch. They are weaker than in a standard model, that is, a model with massless neutrinos, and this lowers the predicted small-scale anisotropy of the relic radiation.

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