In the paper we consider the macroscopic model of plasma of scalar charged particles, obtained by means of the statistical averaging of the microscopic equations of particle dynamics in a scalar field. On the basis of kinetic equations, obtained from averaging, and their strict integral consequences, a self-consistent set of equations is formulated which describes the self-gravitating plasma of scalar charged particles. It was obtained the corresponding closed cosmological model which also was numerically simulated for the case of one-component degenerated Fermi gas and twocomponent Boltzmann system. It was shown that results depend weakly on the choice of a statistical model. Two specific features of cosmological evolution of a statistical system of scalar charged particles were obtained with respect to cosmological evolution of the minimal interaction models: appearance of giant bursts of invariant cosmological acceleration Ω at the time interval 8 · 10 3 ÷ 2 · 10 4 t P l and strong heating (3 ÷ 8 orders of magnitude) of a statistical system at the same times. The presence of such features can modify the quantum theory of generation of cosmological gravitational perturbations. keywordsphysics of the early universe, particle physics -cosmology connection, inflation, phantom scalar interaction
Based on one the authors' approach to a macroscopic description of the scalar interaction, we develop a macroscopic model of a relativistic plasma with a phantom scalar interaction of elementary particles. In this model, as opposed to previous models, the restriction of nonnegativity of the particles' effective mass is removed.
Based on the authors' approach to the macroscopic description of scalar interactions, this paper develops a macroscopic model of a relativistic plasma with phantom scalar interaction of elementary particles. In this paper, macroscopic equations for a statistical system with scalar interaction of particles are obtained, and a complete set of macroscopic equations describing cosmological models is built.
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