Non-Adiabatic Behaviour of the Early Cosmic Baryons Due to Vacuum Pressure Action: What Causes the Structure Formation in the Post-Recombination Era?

In preceding papers we have shown that an initial Big-Bang explosion of the universe can not have happened as simply caused by a singularity of extremely hot, highly condensed cosmic matter due to the enhanced centripetal gravity field, enhanced by relativistic cosmic masses [1-3]. Instead, as we argue here, the initial "Bang" must have started from a pressurized cosmic vacuum. We analyse how to adequately describe this cosmic vacuum pressure and how to formulate the initial scale expansion of the universe as a reaction to it. We find that for a needed positive vacuum pressure the thermodynamic polytrope relation between vacuum energy density and vacuum pressure only allows for a range of the vacuum polytrope indices ξ of 3 ˂ ξvac ˂ 5. Furthermore we find that for the preferred value ξvac = 4 one can derive a complete description of the cosmic vacuum energy as function of the cosmic scale and the cosmic time with inclusion of a process of cosmic matter generation by a specific vacuum condensation process producing quantized matter. As result one obtains a matter universe well acquainted to all present day astronomers, however, without the need for an initial, material Big-Bang of a mass singularity. As a surprise, however, the Hubble expansion of the post-recombination universe under the action of cosmic vacuum pressure drives the baryonic distribution function into a more and more non-equilibrium shape with over-Maxwellian-ized populations of the high velocity wings demonstrating surprisingly enough that the cosmic matter temperatures in this expansion phase are in fact increasing, opposite to classical expectations which properly speaking would clearly predict adiabatic temperature decreases.