A Cosmological Model Based on a Quadratic Equation of State Unifying Vacuum Energy, Radiation, and Dark Energy
Figure 19
Evolution of the temperature of the “generalized” radiation as a function of time in logarithmic scales. Before the early inflation, the universe is extremely cold (). During the early inflation, the temperature increases by orders of magnitude in less than . During the radiation era, the temperature decreases algebraically. The present value of the temperature is (bullet). During the late inflation, the temperature decreases exponentially rapidly.
