twin universe cosmology astrophysics of ghost matter.3 : The radiative era : The problem of the "origin" of the universe.
The problem of the homogeneity of the early universe. (p5) **
Fig. 4 : Evolution of the Planck constant during the radiative era.**
If we plot the curve together :
Fig. 5 : The radiative era. ** **
...This is a new description of the radiative era. The era (t < tcr) corresponds to the primeval universe and nucleosynthesis phenomena. As the energies are assumed to be constant during this period, all associated processes (nucleosynthesis) should be rephrased in terms of "variable constants".
...What about the recombination? Call td the value of time when recombination occurs (in the standard model »105 years). Assume tcr £ td /10. Then, when t > 10 tcr the constants behave like absolute constants. The individual energies of particles are no longer constant and the mixture temperature becomes less than 3000°. Recombination occurs, matter and radiation decouple, etc.
What about the cosmic background radiation?
...In that new description of the radiative era, the photon energy is constant when t < tcr. But the cosmic background radiation photons are not "primeval photons" but "secondary ones", emitted at the recombination time. For t > td their energy falls down and Tr tends to 2,7°K.
...In order to compare the standard model to that new one, call Rcr the value of the space scale factor when t = tcr and Rd its value when t = td (recombination).
** ** Fig. 6 : Compared evolutions : matter and radiation densities.
Similar curves, for matter dominated era and ghost universe
(rm » 1/R3 and rr » 1/R4). **Fig. **7 : This figure is identical to figure 1 except R » t2/3 **during the (short) radiative era **(instead t1/2).
...After the transition, before ghost matter clumps formation (see paper [7]) ,matter temperature Tm » 1/R2, (while Tm » 1/R2) . If we assume an isentropic expansion :
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