Scalar field perturbations in fresh inflation

The model of fresh inflation with increasing cosmological parameter provides sufficient e-folds to solve the flatness/horizon problem and the density fluctuations agree with experimental values. In this model the temperature increases during inflation and reach its maximum value when inflation ends (where the number of e-folds is $N(t_e)\gg 60$). The most important characteristic of this model is that provides a natural transition between the end of inflation and the epoch when the universe is radiation dominated.