Dynamics of polynomial Chaplygin gas warm inflation

Jawad, Abdul; Chaudhary, Shahid; Videla, Nelson

doi:10.1140/epjc/s10052-017-5377-5

Cited by 12 publications

(3 citation statements)

References 66 publications

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“…They studied the model for various types of Ω (dissipation parameter) and ξ (bulk parameter) and reported that the scalar spectral index (n s ) lies in the compatible range for less number of e-folds (N). The authors in [38] investigated the polynomial WI and confirmed the consistency of their results with recent astrophysical data. Sadjadi and Goodarzi [39] discussed oscillatory type of inflation with non-minimal kinetic coupling as a resolution of few number of e-folds ("non-minimal derivative coupling model [40]").…”

Section: Introductionsupporting

confidence: 63%

Inflationary solution of Hamilton Jacobi equations during weak dissipative regime

Saleem

Zubair

2020

Phys. Scr.

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In this paper, an elegant mathematical approach is introduced to solve the equations of warm inflationary model without using extra approximations other than slow-roll. This important inflationary method known as Hamilton-Jacobian formalism. Here tachyon field and the imperfect fluid are considered to be the cosmic ingredients to create inflation. A general formalism is developed for the considered inflationary model and further work is restricted to weak dissipative regime. A detailed analysis of the model is presented for three different choices of bulk and dissipative coefficients taking as constant as well as variable (function of Hubble parameter and inflaton). In each case, the involved model parameters are constrained to plot the physical acceptable range of scalar spectral index and tensor to scalar ratio. The parametric trajectories proved that the acquired results for all the three cases are compatible with Planck astrophysical data. Furthermore, the existence of warm inflation and slow-roll limit are also verified graphically.

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Section: Introductionsupporting

confidence: 63%

Inflationary solution of Hamilton Jacobi equations during weak dissipative regime

Saleem

Zubair

2020

Phys. Scr.

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“…(36) and (37), then necessarily the dissipative coefficient should be given by expression (44). The dissipation coefficient for large √ ξφ can be approximated to…”

Section: The Weak Regimementioning

confidence: 99%

Reconstructing warm inflation

Herrera

2018

Eur. Phys. J. C

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The reconstruction of a warm inflationary universe model from the scalar spectral index n S (N ) and the tensor to scalar ratio r (N ) as a function of the number of e-folds N is studied. Under a general formalism we find the effective potential and the dissipative coefficient in terms of the cosmological parameters n S and r considering the weak and strong dissipative stages under the slow roll approximation. As a specific example, we study the attractors for the index n S given by n S − 1 ∝ N −1 and for the ratio r ∝ N −2 , in order to reconstruct the model of warm inflation. Here, expressions for the effective potential V (φ) and the dissipation coefficient (φ) are obtained.

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“…In the context of warm inflation, the generation of radiation remains quasi-stable, i.e., and , as derived in [26,27]. Therefore, under the slow-roll approximation, the equations of motion can be expressed as…”

Section: Introductionmentioning

confidence: 99%

Chaplygin gas inspired warm inflation and swampland conjectures through various scalar potentials

Jawad,

Azhar,

Sadiq

et al. 2024

Chinese Phys. C

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In this paper, we investigate the inflationary parameters andswampland conjectures in the presence of scalar field and Chaplyginmodels. We examine the inflationary parameters, such as slow-rollparameters, the scalar power spectrum, tensor power spectrum,spectral index and the tensor to scalar ratio in the presence ofscalar field and Chaplygin gas models. We also discuss the recentlyproposed swampland conjectures. We consider that the inflationaryexpansion is driven by a standard scalar field with a decay ratio$\Gamma$ that has a generic power law dependence on the scalar field$\phi$ and the temperature of the thermal bath $T$ is given by$\Gamma(\phi,T)= C_{\phi} \frac{T^{a}}{\phi^{a-1}}$, where$C_{\phi}$ is a dimensionless parameter and $a$ is the inflationdecay rate. Assuming that our model bends in a strong dissipativeregime $(R\gg1)$, we study the background and perturbative dynamicsand obtain the most relevant inflationary observables, such as thescalar power spectrum $\mathcal{P_{R}}$, scalar spectral index$n_{s}$, dissipative ratio $R$, the tensor-to-scalar ratio $r$,running of the scalar spectral index $\frac{dn_{s}}{d\ln{k}}$ andthe generalized ratio of the Swampland de-Sitter conjecture$\frac{\acute{T}V}{\acute{V}T}$ for three different potentials.

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Dynamics of polynomial Chaplygin gas warm inflation

Cited by 12 publications

References 66 publications

Inflationary solution of Hamilton Jacobi equations during weak dissipative regime

Inflationary solution of Hamilton Jacobi equations during weak dissipative regime

Reconstructing warm inflation

Chaplygin gas inspired warm inflation and swampland conjectures through various scalar potentials

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