Chaplygin gas braneworld inflation according to WMAP7 data

Abstract

We consider a Chaplygin gas model with an exponential potential in framework of braneworld inflation. We apply the slow-roll approximation in the high-energy limit to derive various inflationary spectrum perturbation parameters. We show that the inflation observables depend only on the e-folding number N and the final value of the slow-roll parameter e(end). Whereas for small running of the scalar spectral index dns/dlnk, the inflation observables are in good agreement with recent WMAP7 data.Comment: 5 pages, 3 figure

Intermediate-generalized Chaplygin gas inflationary universe model

“…[30]). In this context, it continues unchanged in Chaplygin inflation [20,31]. In this form, the power spectrum related to curvature spectrum, could be written as P R ≃ ζ 2 .…”

“…In order to write down values that relate the tensor to scalar ratio and the spectral index, we numerically solved Eqs. (27), (29), (30) and (31). Again as before, we have used the values A ≃ 2.635 × 10 −2 , ρ Cho = 1, f = 1/2 and κ = 1.…”

Warm intermediate inflationary Universe model in the presence of a generalized Chaplygin gas

“…, where ρ m corresponds to the matter energy density and ρ φ corresponds to the scalar field energy density [37]. In this form, the effective Friedmann equation from the GCG may be viewed as a variant of gravity, which is of great interest in the study of the early Universe motivated by string/M-theory [41][42][43][44].…”

“…(1), and therefore as a fluid representation, but rather, recognize the energy density of matter as the contribution of the energy density associated with a standard scalar field. From this perspective we will obtain a modified Friedmann equation, and we will analyze the GCG as a representation of the variant of gravity [37]. From this modification itself, we will study the warm inflation scenario, and we will consider this model to present dissipative effects coming from an interaction between a standard scalar field and a radiation field.…”

“…(2) can be extrapolate in the Friedmann equation to study an inflationary scenario [37]. In this extrapolation, we identify the energy density of matter with the contribution of the energy density associated to the standard or tachyonic scalar field [32,[38][39][40].…”