Formation of the hydrogen line 21-cm in Dark Ages and Cosmic Dawn: dependences on cosmology and first light

We analyse the formation of the redshifted hyperfine structure line 21-cm of hydrogen atom in the Dark Ages, Cosmic Dawn, and Reionization epochs. The evolution of the global differential brightness temperature in this line was computed to study its dependence on the values of cosmological parameters and physical conditions in the intergalactic medium. Variations of the depth of the Dark Ages absorption line at z similar to 80 with variations of the cosmological parameters Omega(b), Omega(cdm), Omega(Lambda), Omega(K), and H-0 are studied. The standard model with post-Planck parameters predicts a value of the differential brightness temperature in the centre of the absorption line similar to 30-50 mK. The profile of this line can be quite another in the non-standard cosmological models, which include the annihilating or decaying dark matter, a primordial stochastic magnetic field, etc. It can be shallower or be an emission bump instead of an absorption trough. It is also shown that the position and depth of the Cosmic Dawn absorption line formed at 10 < z < 30, due to the Wouthuysen-Field effect, is mainly defined by the spectral energy distribution of the first sources of light. If reionization occurs at z(ri )= 7 +/- 1, then the differential brightness temperature in the centre of this line is similar to 80 mK. During the reionization, the emission with an amplitude of similar to 20 mK is possible. It is also shown that the temperature, density, and degree of ionization of the baryonic component are decisive in calculating the intensity of the 21-cm absorption/emission line from these epochs.