interactions are given by the charged and neutral Currents, coupling the SM fermions to gauge bosons through the J ± µ , J Z µ currents, and the Yukawa sector, and coupling the SM fermions with the Higgs: One can redefine the fields and masses with a specific conformal weight as to keep the canonical kinetic terms for the gauge fields and fermions, provided: ˜ W ± µ ≡ W ± µ / Ω, ˜ Z$_{µ}$ ≡ Z$_{µ}$/ Ω, ˜ ψ$_{d}$ ≡ ψ$_{d}$/ Ω 3 / $^{2}$, ˜ ψ$_{u}$ ≡ ψ$_{u}$/ Ω 3 / $^{2}$, ˜ m 2 W = ˜ m 2 Z cos $^{2}$θ$_{W}$ = m 2 $_{W}$/ Ω 2 = ( g 2 $_{2}$M 2 $_{P}$/ 4 ξ )(1 − e − ακ | χ | ), ˜ m$_{f}$ ≡ m$_{f}$/ Ω = ( y$_{f}$M$_{P}$$^{$_{/}$√$_{2}$$_{ξ}$$_{)}$}$( 1 − e − ακ | χ | ) 1 / $^{2}$, where Ω 2 ≈ exp( ακχ ) with α = √ 2 / 3 and κ = 1 /M$_{P}$ . The oscillations of the Higgs field can be approximated by a simple quadratic potential U ( χ ) ≈ (1 / 2) M $^{2}$χ$^{2}$, where M = √ λ/ 3 M$_{P}$/ξ ∼ 10 − $^{5}$M$_{P}$ . The oscillations evolve with χ ( t ) ≈ X ( t ) sin( Mt ), where X ( t ) ∝ ( Mt ) − $^{1}$, like in the matter- dominated case. There is a small departure from a quadratic potential, which is given by Eq. (215), U ( χ ) = (1 / 2) M $^{2}$χ2 + Δ U ( χ ), but during reheating this correction is negligible. As χ passes through the minimum, by virtue of its couplings, the gauge fields and fermions become massless, therefore they can be excited through parametric resonance or via instant preheating during every oscillations $^{88}$. However during one cycle of oscillation, the gauge bosons and fermions become heavy, as χ goes away from the minimum and obtains a time dependent VEV. During this epoch the gauge fields can decay into lighter fermions, but there is a kinematical blocking. The process of preheating is not as efficient as one would have thought. Nevertheless, the Higgs energy can be transferred at a faster rate compared to that of the perturbative decay of the Higgs, as shown in the Fig. (21) [124]. Furthermore, in order to obtain a full thermalization, Higgs must decay completely, which happens in a time scale similar to that of a perturbative decay rate. Reheating, preheating and thermalization issues are quite different once SUSY is intro- duced. SUSY introduces new degrees of freedom and new parameters. Cosmology also acts C. SUSY generalization of reheating and preheating 88 This feature was first discussed in the context of MSSM inflation, where instant preheating excites the gluons abundantly near the point of enhanced gauge symmetry [89]. 191 S$_{SSB}$ = ∫ d 4 $_{x}$√ − g { m 2 $_{W}$W + µ W µ − + 1 2 m 2 $_{Z}$Z$_{µ}$ Z µ } , S$_{Y}$ = ∫ d 4 $_{x}$√ − g { m$_{d}$ ¯ ψ$_{d}$ψ$_{d}$ + m$_{u}$ ¯ ψ$_{u}$ψ$_{u}$ } , S$_{CC}$ + S$_{NC}$ = ∫ d 4 $_{x}$√ − g { g$_{2}$ √$_{2}$ W + µ $_{J}$− µ + g$_{2}$ √$_{2}$ $_{W}$− µ J + µ + g$_{2}$ cos θ$_{W}$ Z$_{µ}$J µ Z } . (411)