Neutrino cooling effect of primordial hot areas in dependence on its size

Hot Primordial Regions with Anomalous Hydrogenless Chemical Composition

“…They may play a dominant role within a wide range of the region parameters which are specified below. We have shown earlier [23,24], that neutrino emission can be decisive in the temperature evolution of such regions at the first stage. Here we extend consideration by involving reactions with the lightest element formation.…”

“…We can estimate the abundance of (free) neutrons and protons numerically using Equations ( 21) and (22). Figure 2 shows the evolution of the number densities, while Figure 3 shows the fraction of protons (left) or neutrons (right) from the initial baryon number density.…”

“…The matter inside areas can be heated or cooled by various processes acting at the same time. These processes include neutrino cooling [21,22], inelastic reactions between elementary particles and nuclei, the radiation from star-forming hot plasma [1], the gravitational dynamics of the system, the shock waves and diffusion of matter during the region formation [23,24], energy transfer from collapsing walls as mentioned above [14][15][16]25,26], accretion [1,24], and Hawking evaporation [24,27,28]. We focus here on the pure effect of inelastic reactions between elementary particles and nuclei.…”