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Since it is commonly believed that the observed large-scale structure of the
Universe is an imprint of quantum fluctuations existing at the very early stage
of its evolution, it is reasonable to pose the question: Do the effects of
quantum nonlocality, which are well established now by the laboratory studies,
manifest themselves also in the early U...
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Citations
... where w parameterizes the effective equation of state of the cosmological matter, p = wρ (w = 0 for the non-relativistic matter, and w = 1/3 for the radiation); and T (η 0 ) is the age of the Universe. As a result, one should expect that, for example, the observed CMB radiation will be strongly anisotropic (if t * is associated with the instant of recombination), or a large number of topological defects will be formed at the boundaries between the domains [16][17][18][19] (if t * is associated with the instant of phase transition). The situation changes radically if the inflationary stage with exponential expansion is present. ...
An extended non-local field equations characterised by modified dispersion relations have been constructed based on non-local differential and hyperdifferential quantum operators. The dispersion relations obtained are found to be comparable to those obtained within the framework of unified theories and the covariant Kempf–Mangano algebra but free from tachyons. For the case of neutral meson, the upper limit of the characteristic length scale was found to be very close to the nuclear radius obtained from the study of \(\beta ^{+} \)-decay energy from finite-sized nuclei.
