content_image/357248.jpg content_image/357256.jpg content_image/357257.jpg content_image/357258.jpg content_image/357259.jpg
minimal K¨ ahler potential $^{66}$. Then the scalar potential reads 

<img src='content_image/357248.jpg'>

where g$_{ξ}$ is the gauge coupling of U (1)$_{ξ}$. Here, we have assumed a minimal K¨ ahler potential K = | $^{φ}$− | 2 + | φ$_{+}$ | 2 + | S | $^{2}$. The global minimum of the potential is obtained for 〈 S 〉 = 0 and 〈 $^{Φ}$− 〉 = √$_{ξ}$$_{, which is SUSY preserving but induces the breaking of}$ U (1)$_{ξ}$. For S > S$_{inst}$ ≡ $_{g$_{ξ}$}$√$_{ξ/λ}$ the potential is minimized for | φ$_{+}$ | = | $^{φ}$− | = 0 and therefore, at the tree level, the potential exhibits a flat inflationary valley, with vacuum energy V$_{0}$ = g 2 $_{ξ}$ξ $^{2}$/ 2. The radiative corrections depend on the splitting between the effective masses of the components of the superfields Φ$_{+}$ $^{and Φ}$−, because of the transient D -term SUSY breaking. Extracting the quadratic terms from the potential Eq. (248), the scalar components φ$_{+}$ and $^{φ}$− get squared masses: 2 

while the squared mass of the Dirac fermions reads 

<img src='content_image/357256.jpg'>

<img src='content_image/357257.jpg'>

The radiative corrections are given by the Coleman-Weinberg expression [360] and the full potential inside the inflationary valley reads 

<img src='content_image/357258.jpg'>

with 

<img src='content_image/357259.jpg'>

Inflation ends when the slow-roll conditions break down, that is for z$_{end}$ ≃ 1, and the predictions for the inflationary parameters are very similar to the previous discussion on 

