4.4 “End of Inflation” Mechanism 68 From our potential, Eq. (4.2), we have Substituting the VEV of φ , Eq. (4.7), into here gives for all reasonable values of n . Therefore, we require In order that ψ acquires classical perturbations during primordial inflation, we require the effective mass of ψ to be light during this time, i.e. where we are using notation such that | m$_{ψ,}$$_{eff}$ | ≡ √ ∣ m 2 ψ, eff ∣ . We have Therefore we require m 2 ψ, eff = m 2 ψ + ( 4 α 2 − 2 α ) h $^{2}$φ2 ( ψ M$_{P}$ ) 2 α − 2 (4.87) m$_{ψ}$ ≪ $^{H}$∗ (4.88) | m$_{ψ,}$$_{eff}$ | ≪ $^{H}$∗ (4.86) m$_{0}$ ≳ 1 TeV (4.85) m$_{φ,}$$_{now}$ ∼ m$_{0}$ (4.84) m 2 φ, now ∼ − m 2 $_{0}$+ (2 n + 4)(2 n + 3) λ 〈 φ 〉 2 n +2 M 2 n P (4.83) 4.4.3.4 Light ψ