Scalar field perturbations in fresh inflation

Details Scalar field perturbations in fresh inflation Scalar field perturbations in fresh inflation

2003-06-15

arxiv.org/abs/hep-ph/0306131v1

Nuovo Cim. B118 (2003) 417-423

Physics

High Energy Physics

High Energy Physics - Phenomenology

4pages, 3 figures

Scientific paper

10.1393/ncb/i2003-10022-7

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.

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