/8$. The coefficient $K$ varies in the range from $K\simeq 0.2$ at characteristic energies of the nucleosynthesis, $T\sim 10^{-(3\div 4)}$ GeV, to $K=0.025$ at the energies $\sim 10^{2\div 3} GeV$ at which all the standard model degrees of freedom are relativistic. In this range the ratio $\r/\m$ changes from $10^{-22\div 29}$ to $10^{(-3\div 
1)}$. Expression (\[f8\]) can be written as ł[f9]{} =K()\^2 e\^[5y]{} ,where $ HB/\m\simeq 9.1 (\r/\m)^{1/2}$. In the region $y<\b{y}$, where $e^{2\m\b{y}}=1+2\m/\r$, for $\m/\r \ll 1$, we have $$\f{\k^2 \c{T}^0_0 (y,t)}{3\m^2}<C K\left(\f{\r}{\m}\right)^2
,$$ where $C=O(1)$. Fixing $t_l$ so that $\r(t_l)/\m\ll 1$, the ratio (\[f8\]) can be made arbitrary small.

Integrating Eq.(\[5\]), we obtain the (04) component of the Einstein equations as ł[f10]{} =(0,t) .Using the formulas of Sect.7, we have ł[f12]{} \_0\^y dy’= \_0\^y dy’\
= \_0\^y e\^[4y’]{} {-(e\^[y’]{}-1)}dy’ .In the period of late cosmology, using the approximate metric (\[24\]), we can set $\dot{a}(y' ,t)/a(y' ,t)\simeq H(t)$. The factor at the integral (\[f12\]) is ł[f13a]{} = ()\^2()\^[3/2]{} K()\^[3/2]{} . At the temperatures of the Universe of order $10^{-3} GeV$, we have $A=18,\,g_* =10.75$ and $K\simeq 0.12$. At the temperatures at which all the Standard model degrees of freedom are relativistic, $K\simeq 0.011$. The integral in (\[f12\]) is $$I=\int_1^{e^{\m 