Fundamentals of Cosmology

If the early Universe contained only known standard-model particles, then g_b = 28 and g_f = 90, so the temperature at the big bounce was Eq. (28).

“If we assume that the early Universe contained only known standard-model particles, then g b = 28 and g f = 90 [18], so the temperature at the big bounce (16) was”

Cosmic inflation is supported by measurements of the inhomogeneities of the cosmic microwave background radiation.

“Cosmic inflation, which is supported by the measurements of the inhomogeneities of the cosmic microwave background radiation (Rich 2001), also solves the flatness and horizon problems, but it requires additional matter fields with specific conditions on their form and does not address the big bang singularity (Kazanas 1980;Guth 1981;Linde 1982).”

The spin fluid in the early universe is formed by ultrarelativistic matter in kinetic equilibrium, for which ρ = h(T)T^4, p = ρ/3, and n = h_n(T)T^3.

“The spin fluid in the early universe is formed by ultrarelativistic matter in kinetic equilibrium, for which   = T h T 4 ( ) , /  = p T T 3 ( ) ( ) , and = n T h T n 3 ( ) , where T is the temperature of the universe and ζ is the Riemann zeta function, and we defined (Rich 2001).”