Λ-INFLATION AND CMB ANISOTROPY

Abstract

We explore a broad class of three-parameter inflationary models of the very early Universe, called the Λ-inflation, and its observational predictions: high abundance of cosmic gravitational waves consistent with the Harrison–Zel'dovich spectrum of primordial cosmological perturbations, the non-power-law winglike spectrum of matter density perturbations, and others. High efficiency of these models to meet observational tests is briefly discussed. We show that a parity contribution of the gravitational waves and adiabatic density perturbations into the large-scale temperature anisotropy, T/S~1, is a common feature of Λ-inflation; the maximum values of T/S (basically not larger than 10) are reached in models where (i) the local spectrum shape of density perturbations is flat or slightly red (nS≲1), and (ii) the residual potential energy of the inflaton is near the GUT scale [Formula: see text]. The conditions to get large T/S in the inflationary paradigm and the relation of T/S to the ratio of the power spectra, r, and to the inflationary γ and Hubble parameters, are discussed. We argue that a simple estimate, [Formula: see text], is valid for most known inflationary solutions and allows to relate straightforwardly the important parameters of observational and physical cosmology.