content_image/371258.jpg content_image/371259.jpg content_image/371260.jpg content_image/371261.jpg content_image/371262.jpg content_image/371263.jpg content_image/371264.jpg content_image/371265.jpg content_image/371266.jpg content_image/371267.jpg
where α 2 ≪ 1, there exists a point of inflection in V ( φ ) 

at which 

From now on we only keep the leading order terms in all expressions. Note that in gravity- mediated SUSY breaking, the A -term and the soft SUSY breaking mass are of the same order of magnitude as the gravitino mass, i.e. m$_{φ}$ ∼ A ∼ m$_{3}$$_{/}$$_{2}$ ∼ (100 GeV − 1 TeV). Therefore the condition in Eq. (318) can indeed be satisfied. We then have φ$_{0}$ ∼ O (10 14 GeV). Inflation occurs within an interval 3 

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in the vicinity of the point of inflection, within which the slow-roll parameters ϵ ≡ ( M 2 $_{P}$/ 2)( V ′ /V ) 2 and η ≡ M 2 $_{P}$( V ′′ /V ) are smaller than 1. The Hubble expansion rate during inflation is given by 

The amplitude of density perturbations δ$_{H}$ and the scalar spectral index n$_{s}$ are given by [87, 88, 711, 712]: 

and 

respectively where 

N$_{Q}$ is the number of e-foldings between the time when the observationally relevant perturba- tions are generated till the end of inflation and follows: N$_{Q}$ ≃ 66 . 9 + (1 / 4)ln( V ( φ$_{0}$ ) /M 4 $_{P}$) ∼ 

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