content_image/369758.jpg content_image/369760.jpg content_image/369759.jpg content_image/369761.jpg content_image/369762.jpg
K j i = ( K − $^{1}$) j i = δ j $_{i}$) $^{32}$. The kinetic terms for the scalars take the form: 

<img src='content_image/369758.jpg'>

The real part of the gauge kinetic function matrix is given by Re f$_{ab}$ . In the simplest case, it is just a constant, f$_{ab}$ = δ$_{ab}$/g 2 $_{a}$, and the kinetic terms for the gauge potentials, A a $_{µ}$, are given by $^{33}$: 

SUGRA will be broken if one or more of the F$_{i}$ obtain a VEV. The gravitino, spin ± 3 / 2 component of the graviton, then absorb the goldstino component to become massive. Re- quiring classically 〈 V 〉 = 0, as a constraint to obtain the zero cosmological constant, one obtains i 2 

<img src='content_image/369760.jpg'>

<img src='content_image/369759.jpg'>

In case of SUGRA at tree-level with minimal kinetic term, the super-trace formula modifies to (for D -flat directions): 

<img src='content_image/369761.jpg'>

where n$_{φ}$ is the number of the chiral multiplets in the spontaneously broken SUGRA. 

## 1. SUSY generalization of one-loop effective potential 

A SUSY generalization of one-loop effective potential, Eq. (98), is given by [412, 413]: 

<img src='content_image/369762.jpg'>

with Λ$_{c}$ being a momentum cut-off and µ the scale parameter. The renormalized potential will not depend on Λ$_{c}$, and the dots stand for Λ$_{c}$-independent contributions. 

