S. Bilensky's Absolute Values of Neutrino Masses - Status and Prospects PDF

By S. Bilensky

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Let us remind here of the main influences on the power spectrum features and let us leave for later the neutrino mass related issues: 1. , large compared to the horizon scale at recombination), the SW effect dominates the anisotropies. Those are the scales that, at recombination, have had no microphysics processing yet and reflect directly the character and strength of the primordial inhomogeneities. Therefore, one can read from the observed spectrum at large angular scales (small l’s) the general cosmological paradigm about the origin of inhomogeneities.

7 (left panels) and for the “inverted” scheme in Fig. 7 (right panels). For the “normal” scheme with ∆m2sol = ∆m221 , in the case of CP-conservation the allowed values of | m | are constrained to lie in the medium-gray regions a) between the two thick solid lines if η21 = η31 = 1, b) between the two long-dashed lines and the axes if η21 = −η31 = 1, c) between the dash-dotted lines and the axes if η21 = −η31 = −1, d) between the short-dashed lines if η21 = η31 = −1. 05 to the medium-gray regions c) between the solid lines if η21 = η31 = 1, d) between the long-dashed lines if η21 = η31 = −1, e) between the dashed-dotted lines if η21 = −η31 = 1, f) between the short-dashed lines if η21 = −η31 = −1.

1). Relevant for the purposes of this review is the determination of the neutrino mass if the Z-burst mechanism turns out to be the solution to the GZK puzzle, as discussed in Ref. [26] (see also Ref. [228]). A detailed analysis has been done in Ref. [229], where the observed UHE cosmic ray spectrum is compared with the predictions of the Z-burst model. In the analysis one uses collider data to derive the spectra of the final state, and finally one determines the energy losses in the propagation of particles until reaching the Earth atmosphere.

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Absolute Values of Neutrino Masses - Status and Prospects by S. Bilensky


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