The ratio of energy density in relativistic particles thus produced ρ$_{rel}$ with respect to the total energy density ρ$_{0}$ follows from Eqs. (351), (422): where we have used C ∼ O (10). This implies that a fraction ∼ O (10 − $^{1}$) of the inflaton energy density is transferred into relativistic (s)quarks every time that the inflaton passes through the origin. Within 10 − 50 oscillations the inflaton would loose its energy into relativistic MSSM degrees of freedom. • Reheating and thermalization: A full thermal equilibrium is reached when ( a ) kinetic and ( b ) chemical equilibrium are established. The maximum (hypothetical) temperature attained by the plasma would be given by: For instance, if LLe is the inflaton then udd can acquire a large VEV independently. The VEV of udd will spontaneously generate masses to the gluons and gluinos, i.e. To develop and maintain such a large VEV for udd , it is not necessary that udd potential has a saddle point, or point of inflection as well. It can be trapped in a false minimum during inflation, which will then be lifted by thermal corrections when the inflaton decays [89, 136]. The above inequality arises due to the fact that the VEV of ϕ cannot exceed that of the inflaton φ , since its energy density should be subdominant to the inflaton energy density. If gϕ$_{0}$ ≫ T$_{max}$ the gluon/gluino fields will be too heavy and not kinematically acces- sible to the reheated plasma. Here ϕ$_{0}$ is the VEV of udd at the beginning of inflaton oscillations. In a radiation-dominated Universe the Hubble expansion redshifts the flat 161 ρ$_{rel}$ ρ$_{0}$ ∼ $_{10}$− $^{1}$g , (353) T$_{max}$ ∼ V 1 / 4 ∼ ( m$_{φ}$φ$_{0}$ ) 1 / 2 ≈ 10 9 GeV . (354) m$_{G}$ ∼ g 〈 ϕ ( t ) 〉 < gφ$_{0}$ . (355) However, not all the MSSM degrees of freedom can be in thermal equilibrium at such a high temperature. Depending on the nature of a flat direction inflaton, the final reheat temperature can be quite low.