Abstract
We consider an inflationary universe model in the context of generalized cosmic Chaplygin gas by taking matter field as standard and tachyon scalar fields. We evaluate the corresponding scalar fields and scalar potentials during intermediate and logamediate inflationary regimes by modifying the first Friedmann equation. In each case, we evaluate the number of e-folds, scalar as well as tensor power spectra, scalar spectral index and important observational parameter, i.e., tensor-scalar ratio in terms of inflatons. The graphical behavior of this parameter shows that the model remains incompatible with WMAP7 and Planck observational data in each case.
Highlights
A combination of different cosmic probes like type Ia supernova, the large scale structure (LSS), cosmic microwave background (CMB), and WMAP confirmed that our universe is experiencing accelerating expansion [1,2]
Little is known about the origin of this cosmic stage, which may be due to dark energy (DE)
The standard and tachyon scalar fields are considered as the matter con
Summary
A combination of different cosmic probes like type Ia supernova, the large scale structure (LSS), cosmic microwave background (CMB), and WMAP confirmed that our universe is experiencing accelerating expansion [1,2]. Scalar field models composed of kinetic and potential terms coupled to gravity produce a dynamical framework and act as a source for inflation These models have the ability to interpret the distribution of LSS and the observed anisotropy of CMB radiations comprehensively in the inflationary era [30]. The study of warm inflation as a mechanism leads to an end for standard and tachyon inflation This motivated us to consider an inflationary model with these two potentials. Herrera et al [38] studied an intermediate GCG inflationary universe model with standard as well as tachyon scalar fields and checked its compatibility with WMAP7 data. It would be interesting to check the behavior of the inflationary universe with GCCG using the standard and tachyon scalar fields during the intermediate as well as logamediate epochs.
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