The distributions of dissemination pressure and the total pressure of the universe were examined in the general cosmic models in three period intervals. In the limitless epoch t≤ trm, logarithm of two together radiation pressure and the total pressure condescend gradually linearly with record(t). However, in the epoch t = tdec — ty, record(P,(t)) decreases steeply up to t = 6.2104Myr, then it declines evenly until t = 205.9406Myr, therefore it reduces slowly, inasmuch as log(P(t)) decreases fast up to t = 5.9406Myr, following it descends gradually just before t = 112.8713 Myr, where it starts declining moderately. Nevertheless, in the time range t = t, - 50 Gyr, record(P(t)) reduces fast up to t = 1.4458Gyr, then it descends in approximately less rate, while P(t) falls sharply just before t = 0.7229Gyr, hence it declines rapidly until tapp 1.9277Gyr, where P(t) approaches the dark strength pressure P1. As P(t) decreases with limitless time the horizon growth speed of the universe dn(t) descends steadily, while the negative values of the horizon growth acceleration of outer space d(t) increase. On the other hand, the horizon volume speed of outer space expansion V(t) ascends accompanying decreasing P(t), whereas the skyline volume spurring of the universe growth V(t) descends. Slightly after t = tapp, Vn(t) increases to its maximum advantage at t = tmax, then it starts dropping steeply with d(t) towards zero. However, at t = t top dn (t) surges prominently towards nothing, whereas (t) fluctuates about this value. The extreme changes in dn(t), dn (t), Vn(t) and (t) following the outstanding decrease in P(t) at t = tapp exhibits forceful dependence of the cosmic movement on the total pressure of the universe.
Author(s) Details:
Fadel A. Bukhari,
Department of Astronomy, Faculty of Science,
King Abdulaziz University, Jeddah, Saudi Arabia.
Please see the link here: https://stm.bookpi.org/FRAPS-V3/article/view/10373
