4.2 The Model 50 V = 0 at the VEV. 4 V$_{0}$ is obtained by inserting the VEV into the zero temperature potential and then looking along the ψ =0 direction. We obtain We use the Friedmann equation giving the energy density of the Universe during thermal inflation to obtain the Hubble parameter during thermal inflation as V$_{0}$ ∼ ( m 2 n +4 0 M 2 n P λ ) 1 n +1 (4.8) M 2 $_{P}$H 2 TI ∼ V$_{0}$ (4.9) H$_{TI}$ ∼ ( m n +2 0 √$_{λM}$$_{P}$ ) 1 n +1 (4.10) Within this model, we will consider two cases regarding the decay rate of the inflaton, Γ$_{ϕ}$ , with ϕ , the inflaton, being the field driving the period of primordial inflation prior to thermal inflation. Firstly, the case that Γ$_{ϕ}$ ≳ H$_{TI}$ , i.e. that reheating from primordial inflation occurs before or around the time of the start of thermal inflation. Secondly, we will consider the case that Γ$_{ϕ}$ ≪ H$_{TI}$ , i.e. that reheating from primordial inflation occurs at some time after the end of thermal inflation. In the case of Γ$_{ϕ}$ ≳ H$_{TI}$ , thermal inflation will begin at a temperature T$_{1}$ ∼ V 1 4 0 (4.11) $^{4}$We are ignoring a cosmological constant as it is negligible. Considering it would give V =0 at the VEV.