scholarly journals Cosmological test of an extended quintessence model

2021 ◽  
Vol 103 (10) ◽  
Author(s):  
Gong Cheng ◽  
Fengquan Wu ◽  
Xuelei Chen
Keyword(s):  
Quintessence Model

scholarly journals w d =−1 in interacting quintessence model

2010 ◽  
Vol 66 (3-4) ◽  
pp. 445-449 ◽  
Author(s):  
H. Mohseni Sadjadi
Keyword(s):  
Quintessence Model

Some dynamical aspects of interacting quintessence model

Pramana ◽  
2018 ◽  
Vol 90 (4) ◽  
Author(s):  
Binayak S Choudhury ◽  
Himadri Shekhar Mondal ◽  
Devosmita Chatterjee
Keyword(s):  
Quintessence Model

scholarly journals QUINTESSENCE AND THE FIRST DOPPLER PEAK

2001 ◽  
Vol 16 (31) ◽  
pp. 2003-2011 ◽  
Author(s):  
PEDRO F. GONZALEZ-DIAZ
Keyword(s):  
Topology Of The Universe ◽  
The Universe ◽  
Quintessence Model

By using a tracking quintessence model we obtain that the position of the first Doppler peak in the spectrum of CMB anisotropies only depends on the topology, of the universe, Ωk, for any value of the ratio ΩΛ/ΩM, so that such a dependence is perfectly valid in the range suggested by supernova observations. A prediction from the used quintessence model is also that all peaks at positions ℓn for n even are fully suppressed on that spectrum.

scholarly journals On the Higgs-like quintessence for dark energy

2014 ◽  
Vol 29 (22) ◽  
pp. 1450117 ◽  
Author(s):  
Sergei V. Ketov ◽  
Natsuki Watanabe
Keyword(s):  
Dark Energy ◽  
Cosmological Constant ◽  
Scalar Curvature ◽  
Scalar Potential ◽  
Fine Tuning ◽  
Standard Description ◽  
Quintessence Model

We propose a dynamical (quintessence) model of dark energy in the current Universe with a renormalizable (Higgs-like) scalar potential. We prove the viability of our model (after fine-tuning) for the certain range of the average scalar curvature values, and study the cosmological signatures distinguishing our model from the standard description of dark energy in terms of a cosmological constant.

scholarly journals COUPLING OF QUINTESSENCE TO PSEUDOSCALAR OF ELECTROMAGNETISM AND CMB POLARIZATION

2007 ◽  
Vol 22 (25n28) ◽  
pp. 1953-1958
Author(s):  
GUO CHIN LIU
Keyword(s):  
Cosmic Microwave Background ◽  
Power Spectra ◽  
Polarization Plane ◽  
Microwave Background ◽  
Cmb Polarization ◽  
Quintessence Model

Coupling between quintessence and pseudoscalar of electromagnetism induces the rotation of the polarization plane of Cosmic Microwave Background(CMB). This rotation mixes the power between E and B modes and generates parity-violating TB and EB modes. Given the potential of a quintessence model, we present the full set of CMB power spectra for temperature and polarization anisotropies. These power spectra can be used to constrain the coupling and quintessence model.

scholarly journals QUINTESSENCE MODEL BUILDING

2002 ◽  
Author(s):  
P. BRAX ◽  
J. MARTIN ◽  
A. RIAZUELO
Keyword(s):  
Model Building ◽  
Quintessence Model

scholarly journals A dark energy quintessence model of the universe

2019 ◽  
Vol 35 (04) ◽  
pp. 2050002
Author(s):  
G. K. Goswami ◽  
Anirudh Pradhan ◽  
A. Beesham
Keyword(s):  
Dark Energy ◽  
Deceleration Parameter ◽  
Cosmological Parameters ◽  
Hubble Constant ◽  
Time Dependent ◽  
Observational Constraints ◽  
History Of ◽  
Flrw Universe ◽  
The Universe ◽  
Quintessence Model

In this paper, we have presented a model of the Friedmann–Lemaitre–Robertson–Walker (FLRW) universe filled with matter and dark energy (DE) fluids by assuming an ansatz that deceleration parameter (DP) is a linear function of the Hubble constant. This results in a time-dependent DP having decelerating–accelerating transition phase of the universe. This is a quintessence model [Formula: see text]. The quintessence phase remains for the period [Formula: see text]. The model is shown to satisfy current observational constraints. Various cosmological parameters relating to the history of the universe have been investigated.

scholarly journals Dynamics of quintessence in generalized uncertainty principle

2020 ◽  
Vol 80 (10) ◽  
Author(s):  
Alex Giacomini ◽  
Genly Leon ◽  
Andronikos Paliathanasis ◽  
Supriya Pan
Keyword(s):  
Uncertainty Principle ◽  
Critical Points ◽  
System Analysis ◽  
Field Model ◽  
Generalized Uncertainty Principle ◽  
De Sitter ◽  
Exponential Potential ◽  
Isotropic Universe ◽  
General Potential ◽  
Quintessence Model

AbstractWe investigate the quintessence scalar field model modified by the generalized uncertainty principle in the background of a spatially flat homogeneous and isotropic universe. By performing a dynamical system analysis we examine the nature of the critical points and their stability for two potentials, one is the exponential potential and the other is a general potential. In the case of an exponential potential, we find some new critical points for this modified quintessence scenario that describe the de Sitter universes, and these critical points do not appear in the standard quintessence model with an exponential potential. This is one of the main results of this work. Now for the general potential our analysis shows that the physical properties of the critical points remain exactly the same as for the exponential potential which means that within this modified quintessence scenario all kind of potentials have same behaviour. This kind of result is completely new in cosmology because with the change of the potential, differences are usually expected in all respect.

scholarly journals DILATON COUPLED QUINTESSENCE MODEL IN THE ω - ω′ PLANE

2007 ◽  
Vol 16 (07) ◽  
pp. 1109-1117 ◽  
Author(s):  
Z. G. HUANG ◽  
H. Q. LU ◽  
W. FANG
Keyword(s):  
Dark Energy ◽  
Field Equation ◽  
Scalar Field ◽  
Equation Of State ◽  
State Parameter ◽  
Equation Of Motion ◽  
Gravitational Theory ◽  
Scalar Field Equation ◽  
Equation Of State Parameter ◽  
Quintessence Model

In this paper, we regard the dilaton in Weyl-scaled induced gravitational theory as a coupled quintessence. Based on this consideration, we investigate the dilaton coupled quintessence (DCQ) model in the ω - ω′ plane, which is defined by the equation of state parameter for the dark energy and its derivative with respect to N (the logarithm of the scale factor a). We find the scalar field equation of motion in the ω - ω′ plane, and show mathematically the properties of attractor solutions which correspond to ωσ ~ -1, ωσ = 1. Finally, we find that our model is a tracking one which belongs to "freezing" type models classified in the ω - ω′ plane.

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