Exact inflationary solution in the chaotic inflation model to non-minimally coupled scalar field

2009 ◽  
Vol 87 (11) ◽  
pp. 1181-1184
Author(s):  
Shiwu Chen ◽  
Xizhun Hao ◽  
Xiongwei Liu ◽  
Shuzheng Yang
Keyword(s):  
Scalar Field ◽  
Spectral Index ◽  
Hubble Parameter ◽  
Density Fluctuation ◽  
Minimal Coupling ◽  
Astronomical Observations ◽  
Scalar Density ◽  
Inflation Model ◽  
Exact Inflationary Solution ◽  
Chaotic Inflation

We present a new exact inflationary solution for the chaotic inflation model with non-minimal coupling, by taking the Hubble parameter directly as a function of a scalar field. We then prove that the spectral index of the scalar density fluctuation (and other parameters), which derived from the exact inflationary solution, is exactly consistent with recent astronomical observations.

A Kind of Exact Inflationary Solution in the Chaotic Inflation Model to Non-minimally Coupled Scalar Field

2008 ◽  
Vol 25 (9) ◽  
pp. 3162-3164 ◽  
Author(s):  
Chen Shi-Wu ◽  
Yang Shu-Zheng ◽  
Hao Xi-Zhun ◽  
Liu Xiong-Wei
Keyword(s):  
Scalar Field ◽  
Inflation Model ◽  
Exact Inflationary Solution ◽  
Chaotic Inflation

scholarly journals CHAOTIC INFLATION ON THE RANDALL–SUNDRUM TWO-BRANE MODEL

2010 ◽  
Vol 25 (31) ◽  
pp. 2697-2713
Author(s):  
KOUROSH NOZARI ◽  
SIAMAK AKHSHABI
Keyword(s):  
Scalar Field ◽  
Field Potential ◽  
Friedmann Equation ◽  
Warp Factor ◽  
Model Parameters ◽  
Stabilization Mechanism ◽  
Brane Model ◽  
Inflation Model ◽  
Bulk Scalar Field ◽  
Chaotic Inflation

We construct an inflation model on the Randall–Sundrum I (RSI) brane where a bulk scalar field stabilizes the inter-brane separation. We study impact of the bulk scalar field on the inflationary dynamics on the brane. We proceed in two different approaches: in the first approach, the stabilizing field potential is directly appeared in the Friedmann equation and the resulting scenario is effectively a two-field inflation. In the second approach, the stabilization mechanism is considered in the context of a warp factor so that there is just one field present that plays the roles of both inflaton and stabilizer. We study constraints imposed on the model parameters from recent observations.

scholarly journals TRANS-PLANCKIAN PHYSICS AND NON-COMMUTATIVE INFLATION

2008 ◽  
Vol 23 (17n20) ◽  
pp. 1598-1605 ◽  
Author(s):  
SEOKTAE KOH
Keyword(s):  
Scalar Field ◽  
Thermal Radiation ◽  
Spectral Index ◽  
Planck Scale ◽  
Dispersion Relations ◽  
Scale Invariant ◽  
Inflation Model

Non-commutativity of spacetime at the Planck scale may deform the usual dispersion relations. And these deformed dispersion relations could lead to the accelerating phase without a scalar field. In this paper, we have calculated the spectral index and the running of spectral index in a non-commutative inflation model. Non-commutative inflation with thermal radiation gives a scale invariant spectrum in the limit w → −1 and negative running spectral index which are consistent with the WMAP 3-year results.

scholarly journals A new approach to exact solutions construction in scalar cosmology with a Gauss–Bonnet term

2017 ◽  
Vol 32 (25) ◽  
pp. 1750129 ◽  
Author(s):  
I. V. Fomin ◽  
S. V. Chervon
Keyword(s):  
Scalar Field ◽  
Cosmological Model ◽  
Exact Solutions ◽  
Hubble Parameter ◽  
Inflationary Cosmology ◽  
Friedmann Universe ◽  
Minimal Coupling ◽  
New Approach ◽  
Bonnet Gravity ◽  
Bonnet Term

We study the cosmological model based on Einstein–Gauss–Bonnet gravity with non-minimal coupling of a scalar field to a Gauss–Bonnet term in four-dimensional (4D) Friedmann universe. We show how constructing the exact solutions by the method based on a confrontation of the Hubble parameter in the model under consideration is achieved with that in a standard scalar field inflationary cosmology.

scholarly journals Favored Inflationary Models by Scalar Field Condensate Baryogenesis

Galaxies ◽  
2021 ◽  
Vol 9 (3) ◽  
pp. 49
Author(s):  
Daniela Kirilova ◽  
Mariana Panayotova
Keyword(s):  
Scalar Field ◽  
Baryon Asymmetry ◽  
Inflationary Model ◽  
Inflation Model ◽  
Low Energies ◽  
Inflationary Models ◽  
Chaotic Inflation

We calculate the baryon asymmetry value generated in the Scalar Field Condensate (SCF) baryogenesis model obtained in several inflationary scenarios and different reheating models. We provide analysis of the baryon asymmetry value obtained for more than 70 sets of parameters of the SCF model and the following inflationary scenarios, namely: new inflation, chaotic inflation, Starobinsky inflation, MSSM inflation, quintessential inflation. We considered both cases of efficient thermalization after inflation and delayed thermalization. We have found that the SFC baryogenesis model produces baryon asymmetry orders of magnitude bigger than the observed one for the following inflationary models: new inflation, new inflation model by Shafi and Vilenkin, MSSM inflation, chaotic inflation with high reheating temperature and the simplest Shafi–Vilenkin chaotic inflationary model. Strong diluting mechanisms are needed for these models to reduce the resultant baryon excess at low energies to its observational value today. We have found that a successful generation of the observed baryon asymmetry is possible by the SCF baryogenesis model in Modified Starobinsky inflation, chaotic inflation with low reheating temperature, chaotic inflation in SUGRA, and Quintessential inflation.

scholarly journals FERMIONIC AND SCALAR FIELDS AS SOURCES OF INTERACTING DARK MATTER–DARK ENERGY

2011 ◽  
Vol 20 (13) ◽  
pp. 2543-2558 ◽  
Author(s):  
SAMUEL LEPE ◽  
JAVIER LORCA ◽  
FRANCISCO PEÑA ◽  
YERKO VÁSQUEZ
Keyword(s):  
Dark Matter ◽  
Dark Energy ◽  
Scalar Field ◽  
Analytical Solution ◽  
Scalar Fields ◽  
Nonminimal Coupling ◽  
Field Equations ◽  
Fermionic Field ◽  
Minimal Coupling ◽  
Constant Type

From a variational action with nonminimal coupling with a scalar field and classical scalar and fermionic interaction, cosmological field equations can be obtained. Imposing a Friedmann–Lemaître–Robertson–Walker (FLRW) metric, the equations lead directly to a cosmological model consisting of two interacting fluids, where the scalar field fluid is interpreted as dark energy and the fermionic field fluid is interpreted as dark matter. Several cases were studied analytically and numerically. An important feature of the non-minimal coupling is that it allows crossing the barrier from a quintessence to phantom behavior. The insensitivity of the solutions to one of the parameters of the model permits it to find an almost analytical solution for the cosmological constant type of universe.

scholarly journals NONCOMMUTATIVE DECRUMPLING INFLATION AND RUNNING OF THE SPECTRAL INDEX

2005 ◽  
Vol 14 (03n04) ◽  
pp. 621-633 ◽  
Author(s):  
FOROUGH NASSERI ◽  
S. A. ALAVI
Keyword(s):  
Noncommutative Geometry ◽  
Spectral Index ◽  
Time Variability ◽  
Inflation Model ◽  
Slow Roll ◽  
Spatial Dimensions

We present a new inflation model, known as noncommutative decrumpling inflation, in which space has noncommutative geometry with time variability of the number of spatial dimensions. Within the framework of noncommutative decrumpling inflation, we compute both the spectral index and its running. Our results show the effects of both time variability of the number of spatial dimensions and noncommutative geometry on the spectral index and its running. Two classes of examples have been studied and comparisons made with the standard slow-roll formulae. We conclude that the effects of noncommutative geometry on the spectral index and its running are much smaller than the effects of time variability of spatial dimensions.

scholarly journals PRE-INFLATION IN THE PRESENCE OF CONFORMAL COUPLING

2004 ◽  
Vol 19 (11) ◽  
pp. 807-816
Author(s):  
APOSTOLOS KUIROUKIDIS ◽  
DEMETRIOS B. PAPADOPOULOS
Keyword(s):  
Scalar Field ◽  
Exact Solutions ◽  
Hubble Parameter ◽  
Field Potential ◽  
Critical Value ◽  
Big Bang ◽  
Massless Scalar ◽  
Massless Scalar Field ◽  
Conformal Parameter ◽  
Flrw Universe

We consider a massless scalar field, conformally coupled to the Ricci scalar curvature, in the pre-inflation era of a closed FLRW Universe. The scalar field potential can be of the form of the Coleman–Weinberg one-loop potential, which is flat at the origin and drives the inflationary evolution. For positive values of the conformal parameter ξ, less than the critical value ξ c =(1/6), the model admits exact solutions with nonzero minimum scale factor and zero initial Hubble parameter. Thus these solutions can be matched smoothly to the so-called Pre-Big-Bang models. At the end of this pre-inflation era one can match inflationary solutions by specifying the form of the potential and the whole solution is of the class C(1).

scholarly journals Lower bound of the tensor-to-scalar ratior≳0.1in a nearly quadratic chaotic inflation model in supergravity

2015 ◽  
Vol 741 ◽  
pp. 267-271 ◽  
Author(s):  
Keisuke Harigaya ◽  
Masahiro Kawasaki ◽  
Tsutomu T. Yanagida
Keyword(s):  
Lower Bound ◽  
Inflation Model ◽  
Chaotic Inflation
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