Lambda-inflation and CMB anisotropy

We explore a broad class of three-parameter inflationary models of the very early Universe, called the Lambda-inflation, and its observational predict ions: high abundance of cosmic gravitational waves consistent with the Harr ison-Zel'dovich spectrum of primordial cosmological perturbations, the non- power-law winglike spectrum of matter density perturbations, and others. Hi gh efficiency of these models to meet observational tests is briefly discus sed. We show that a parity contribution of the gravitational waves and adia batic density perturbations into the large-scale temperature anisotropy, T/ S similar to 1, is a common feature of Lambda-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 of slightly red (n(S) less than or similar to 1), and (ii) the residual potential energy of the inflation is near the GUT scale ( v(0)(1/4) similar to 10(16) GeV) The cond itions to get large T/S in the inflationary paradigm and the relation of T/ S to the ratio of the power spectra, r(1) and to the inflationary gamma and Hubble parameters, are discussed. We argue that a simple estimate, T/S sim ilar or equal to 3r similar or equal to 12 gamma similar or equal to ( H/6x 10(13) GeV) (2), is valid for most known inflationary solutions and allows to relate straightforwardly the important parameters of observational and p hysical cosmology.