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5 M. S. Turner, Ibidem, p. 10. 48 Inflationary Cosmology Revisited epoch, that show mass densities and energy densities only very slightly lower or slightly higher than the mean value. The expansions and contractions of such density fluctuations can be viewed as acoustic waves in the viscous elastic cosmic fluid in which, at the end of the plasma epoch, radiation pressure was competing against gravitational contraction. In fact, radiation pressure, dominant in the plasma epoch, can be viewed as the driving force for the cosmic expansion all the way since the Big Bang, at least since Planks epoch (t~10"44s) and conceivably even earlier.
1] (Einstein's Equation) * H *-- ttf. 1] For sufficient early time (sufficient small radius), the first term within the squared root, in which p = M /(^R3), becomes much larger than the second, containing as it does a more pronounced dependence on 1/R than the later. Therefore, the second term is at first irrelevant, which is equivalent to put k=0, making cosmic space apparently flat, even if it is actually either closed, with k>0 (which happens not to be the case) or open, with k<0 (which seems in all appearance to be the case), all throughout its entire history.
Sanchez Gomez, M. A. Alario (Eds), "Cosmologia Astrofisica", pp. 88-89 (Alianza Universidad; Madrid, 1995). Dark Matter, Cosmic Flatness & Accelerated Expansion 27 Fig. 1. Velocity components of the observed CMB Dipole. Fig. 2 shows the microwave map of the sky obtained by the DMRCOBE instruments, showing the anticipated small anisotropies as they were at the time of atom formation, when the universe became transparent, and the very first light4 began to travel almost freely in all ' Ibidem, p.
Bohn On the History of Conservation of Energy and of its Application to Physics