Pilgrim Dark Energy Model Research Articles

Generalized ghost pilgrim dark energy model in f(ℚ,) theory

This study investigates the reconstruction technique for the generalized ghost pilgrim dark energy model within the framework of f(Q,T) gravity ( Q represents the non-metricity and T denotes the trace of the energy-momentum tensor). For this purpose, we implement a correspondence scheme for the configuration of dust fluid within a flat Friedmann-Robertson-Walker universe. We examine the cosmic behavior of the reconstructed model by studying cosmological diagnostic parameters in conjunction with phase planes. The analysis reveals that within certain ranges of free parameters, the equation of state parameter characterizes a phantom regime. The trajectories on the ωDE−ωDE′ plane indicate a freezing region, while the phase plane of r − s corresponds to the Chaplygin gas model. The squared sound speed parameter provides stable model for the evolutionary paradigm of the Universe. It is worth noting that our results closely align with the recent observational data.

Generalized ghost pilgrim dark energy model in Non-Riemannian geometry

In this paper, we analyze cosmic evolution and current expansion using the generalized ghost pilgrim dark energy model for the flat Friedmann-Robertson-Walker universe in f(Q) gravity, where Q represents the non-metricity. For this objective, we examine interacting forms of dark energy model and reconstruct f(Q) gravity in terms of red-shift parameter. We establish various standard cosmological parameters including the equation of state parameter, the squared speed of sound, ωD−ωD′ and r − s-planes to examine the impact of this dark energy model. The analysis reveals that all the reconstructed models exhibit an increasing or decreasing trend in the pilgrim dark energy parameter. The equation of state parameter depicts the phantom era, while the squared speed of sound reveals a stable generalized ghost pilgrim dark energy model for the entire cosmic evolutionary paradigm. Finally, we study the cosmography of the ωD−ωD′ and r − s planes that correspond to the freezing region and Chaplygin gas model, respectively. We conclude that all the outcomes are consistent with the pilgrim dark energy phenomenon.

Interacting generalized anisotropic scalar field models

This paper is devoted to investigate the interacting generalized ghost pilgrim dark energy model in the background of anisotropic universe in general relativity. We analyze the two parameters i.e., hubble parameter and equation of state parameter to explore the cosmological evolution of the Bianchi type universe. We study scalar field dark energy models i.e., quintessence, dilaton, K-essence and tachyon to check the consistency of the current universe with their scalar field and corresponding potentials. Further, we check the compatibility of fractional density of matter and dark energy with recent observations of Plank along with their graphical analysis. It is remarkable to conclude that that both fractional densities admits consistency with Plank data 2018 in all cases of Bainchi type universe.

Study of cosmological evolution via GGPDE f(R) models

This paper examines the cosmic evolution and current expansion for flat FRW universe through generalized ghost pilgrim dark energy model in [Formula: see text] gravity. For this purpose, we reconstruct the models in terms of red-shift parameter with respect to three scale factors, i.e. power-law, intermediate and a scale factor defining two unified phases. We study compatibility of reconstructed [Formula: see text] models through [Formula: see text]-[Formula: see text] planes whereas graphical analysis of squared speed of sound leads to investigate their stability. We also explore the behavior of cosmological parameters such as equation of state and deceleration parameters. Moreover, we study the existence of freezing/thawing regions via [Formula: see text]-[Formula: see text] planes. We conclude that squared speed of sound identifies both stability/instability of reconstructed [Formula: see text] models while equation of state and deceleration parameters specifies transition from decelerated to accelerated expanding cosmos. The [Formula: see text]-[Formula: see text] planes discover thawing as well as freezing regions for particular values of pilgrim parameter.

Dynamics of dark energy and scalar field models in non-flat universe

This Paper is devoted to study the effects of different scalar field models under the influence of interacting generalized ghost pilgrim dark energy model in the framework of non-flat FRW universe. For this purpose, we examine the behavior of equation of state and Hubble parameters for two different values of interaction term. Moreover, we consider Lagrangian density of quintessence, tachyon, k-essence and dilaton models to check the consistency of dark energy model with scalar field models. We also evaluate their corresponding potentials and discuss the behavior of kinetic as well as potential energies graphically. We also check the consistency of fractional density of matter and dark energy with Planks 2018.

Evolution of non-flat cosmos via GGPDE f(R) model

This paper is devoted to explore the cosmic evolution of non-flat Friedmann Robertson Walker universe through generalized ghost pilgrim dark energy model in the background of f(R) gravity. For this purpose, we consider two well known scale factors, i.e., power-law and unified scale factors in terms of red shift parameter. For these scale factors, we reconstruct the given dark energy model in f(R) gravity and determine its stability/instability through squared speed of sound parameter. In order to discuss the behavior of reconstructed and dark energy models, we evaluate well known cosmological parameter such as equation of state parameter along with omega –omega ' plane. In addition to this, we also investigate compatibility of new models with standard cosmological models through state-finder parameters. The density parameter is formulated for both ordinary matter as well as dark energy components and results are compared with Planck 2018 constraints. It is concluded that cosmological parameters reveal consistency with recent observations while the value of density parameter suggested by Planck 2018 is achieved by power-law scale factor in most of the cases as compared to unified scale factor.

Viability of specific reconstructed f(T,𝒯 ) models

The reconstruction scenario of well-established dark energy models such as pilgrim dark energy model and generalized ghost dark energy with Hubble horizon and [Formula: see text] models is being considered. We have established [Formula: see text] models and analyzed their viability through equation of state parameter and [Formula: see text] (where prime denotes derivative with respect to [Formula: see text]) plane. The equation of state parameter evolutes the universe in three different phases such as quintessence, vacuum and phantom. However, the [Formula: see text] plane also describes the thawing as well as freezing region of the universe. The recent observational data also favor our results.

A study of pilgrim dark energy model in Brans–Dicke theory

In this paper, we study the behavior of non-interacting and interacting pilgrim dark energy (DE) for non-flat FRW model in Brans–Dicke (BD) theory. We consider the future event horizon as well as logarithmic form of BD scalar field [Formula: see text], where [Formula: see text], [Formula: see text] and [Formula: see text] is the scale factor. We evaluate some well-known cosmological parameters such as equation of state as well as deceleration parameter and [Formula: see text] plane as well as statefinder parameters. We discuss graphical behavior of these parameters through pilgrim DE parameter [Formula: see text] for both non-interacting as well as interacting case with interacting parameter [Formula: see text]. It is found that the equation of state parameter gives consistent results with the current cosmic behavior while the deceleration parameter represents transition from decelerated to accelerated phase. The cosmological planes represent different DE regions. Finally, we discuss stability of the model through squared speed of sound in both cases.

Generalized ghost pilgrim dark energy in f(G,T) gravity

In this paper, we explore the reconstruction paradigm for generalized ghost pilgrim dark energy model with [Formula: see text] gravity ([Formula: see text] is the Gauss–Bonnet invariant and [Formula: see text] is the trace of the energy–momentum tensor) depending upon the speculation of black hole-free universe. To accomplish this, we adopt correspondence scheme for dust fluid configuration with flat Friedmann-Robertson-Walker (FRW) universe. The cosmic behavior of reconstructed models is examined through cosmological diagnostic parameters and phase planes. It is found that the deceleration parameter indicates accelerated phase while equation-of-state parameter represents phantom regime for some specific range of free parameters. The squared speed of sound parameter gives stable models for analyzing evolutionary paradigm of the universe. The trajectories of [Formula: see text]–[Formula: see text] plane gives thawing region, whereas [Formula: see text]–[Formula: see text] phase plane corresponds to Chaplygin gas model. We conclude that the resulting model represents self-consistent phantom-like universe for [Formula: see text] cannot be fraction) as well as stable generalized ghost pilgrim dark energy [Formula: see text] model.

Pilgrim dark energy in f(G, T) gravity

In this paper, we analyze the reconstruction paradigm for pilgrim dark energy model with f(G, T) gravity using Hubble horizon as IR-cutoff. To accomplish this, we use correspondence scheme for dust fluid configuration with flat FRW universe. The cosmological behavior of reconstructed model is examined through cosmic diagnostic parameters and phase planes. It is found that the deceleration parameter indicates accelerated phase while equation of state parameter represents phantom regime. The squared speed of sound parameter gives stable model for analyzing current cosmic evolutionary paradigm. The trajectories of [Formula: see text] plane gives the thawing region, whereas r[Formula: see text]s phase plane corresponds to Chaplygin gas model. We conclude that the resulting model represents aggressive phantom-like universe for u[Formula: see text]0 (with odd choices only), as well as self-consistent PDE f(G, T) model.

Interacting and noninteracting dark energy models in f(R) gravity

In this paper, we study cosmic evolution and current expansion via generalized ghost pilgrim dark energy (PDE) model for FRW universe in [Formula: see text] gravity. For this purpose, we consider both interacting and non-interacting forms of dark energy (DE) model and reconstruct [Formula: see text] model using red-shift parameter. In order to analyze the effects of the DE model, we formulate some standard cosmological parameters such as Hubble, effective equation of state (EoS) and statefinder parameters as well as [Formula: see text]–[Formula: see text] plane. We also investigate the stability criteria for both interacting and noninteracting models through the squared speed of sound. It is concluded that the best-fit results are found for the positive curvature parameter in the presence of the noninteracting model. For the interacting model, the cosmic evolution is well explained by closed and open universe models while the flat geometry effectively describes the current cosmos.

Cosmological study of reconstructed f ( T ) $f(T)$ models

In this paper, we construct \(f(T)\) models by using some dark energy models taking FRW space-time under reconstruction scenario. These dark energy models consist of pilgrim dark energy model with event horizon and Granda-Oliveros as infrared cutoff and higher order time derivatives of Hubble parameter. Using these models we drive the cosmological parameters such as equation of state, square speed of sound and \(\omega_{T}-\omega_{T}'\) plane taking power-law form of scale factor. We discuss these parameters graphically for different values of scale factor parameter. The first and second models represent quintessence and phantom era with stable behavior and freezing region for smaller values of scale factor parameter. The third model shows unstable behavior while phantom era of the universe.

Generalized ghost pilgrim dark energy in F(T,TG) cosmology

This paper is devoted to study the generalized ghost pilgrim dark energy (PDE) model in [Formula: see text] gravity with flat Friedmann–Robertson–Walker (FRW) universe. In this scenario, we reconstruct [Formula: see text] models and evaluate the corresponding equation of state (EoS) parameter for different choices of the scale factors. We assume power-law scale factor, scale factor for unification of two phases, intermediate and bouncing scale factor. We study the behavior of reconstructed models and EoS parameters graphically. It is found that all the reconstructed models show decreasing behavior for PDE parameter [Formula: see text]. On the other hand, the EoS parameter indicates transition from dust-like matter to phantom era for all choices of the scale factor except intermediate for which this is less than [Formula: see text]. We conclude that all the results are in agreement with PDE phenomenon.

Generalized Ghost Pilgrim Scalar Field Models of Dark Energy

We assume generalized ghost Pilgrim dark energy (GGPDE) model in the presence of cold dark matter in flat FRW universe. With suitable choice of interaction term between GGPDE and cold dark matter, we investigate the nature of equation of state parameter for GGPDE. Also, we investigate the natures of dynamical scalar field models (such as quintessence, tachyon, k-essence, and dilaton dark energy) and concerned potentials through the correspondence phenomenon between GGPDE and these models.

Reconstruction of generalized ghost pilgrim dark energy in F ( R ˜ ) $F(\tilde{R})$ gravity

In this paper, we study the reconstruction scenario of a dark energy model in the framework of modified Horava-Lifshitz \(F(R)\) gravity or \(F(\tilde{R})\) gravity. We assume generalized ghost pilgrim dark energy model in flat universe. We consider three well-known scale factors to analyze the behavior of reconstructed \(F(\tilde{R})\) model. These scale factors include bouncing and intermediate scale factors as well as scale factor representing the unification of matter and accelerated phases. The graphical representation is adopted to analyze the behavior of reconstructed model and equation of state parameter for different values of model parameter. The reconstructed model represents increasing and decreasing behavior with respect to time in all cases. The equation of state parameter represents phantom-like universe after transition for intermediate scale factor while quintessence behavior for bouncing and unified scale factors. We also found that the squared speed of sound exhibits the stability of all reconstructed models.

Cosmological Analysis of Dynamical Chern-Simons Modified Gravity via Dark Energy Scenario

The purpose of this paper is to study the cosmological evolution of the universe in the framework of dynamical Chern-Simons modified gravity. We take pilgrim dark energy model with Hubble and event horizons in interacting scenario with cold dark matter. For this scenario, we discuss cosmological parameters such as Hubble and equation of state and cosmological plane likeωϑ-ωϑ′and squared speed of sound. It is found that Hubble parameter approaches the ranges75-0.5+0.5(foru=2) and (74, 74.30) (foru=1,-1,-2) for Hubble horizon pilgrim dark energy. It implies the ranges74.80-0.005+0.005(foru=2) and (73.4, 74) (foru=-2) for event horizon pilgrim dark energy. The equation of state parameter provides consistent ranges with different observational schemes. Also,ωϑ-ωϑ′planes lie in the range (ωϑ=-1.13-0.25+0.24,ωϑ′<1.32). The squared speed of sound shows stability for all present models in the present scenario. We would like to mention here that our results of various cosmological parameters show consistency with different observational data like Planck, WP, BAO,H0, SNLS, and WMAP.

Cosmological reconstruction of pilgrim dark energy model in f(T,T G ) gravity

In this paper, we study f(T,T G ) gravity in FRW spacetime taking into account correspondence scheme. For this purpose, we assume pilgrim dark energy model with event horizon as infrared cutoff. We construct f(T,T G ) model to analyze the behavior of the model as well as evolution trajectories of some cosmological parameters. That is, we study equation of state parameter, squared speed of sound and w PDE – $w'_{\mathit{PDE}}$ analysis taking into account two cases of model parameter. The equation of state parameter in this scenario shows consistency with pilgrim dark energy phenomenon with quintom behavior. The squared speed of sound exhibits stability and instability of the model corresponding to model parameter. We also attain the thawing and freezing regions as well as ΛCDM limits through w PDE – $w'_{\mathit{PDE}}$ plane. Also, we construct a solution by taking ΛCDM model in underlying gravity.

Reconstructing f(R), f(G), f(T), and Einstein-Aether gravities from entropy-corrected (m,n) type pilgrim dark energy

First, we describe the ordinary holographic dark energy (HDE), (m,n) type holographic dark energy, entropy-corrected holographic dark energy (ECHDE) for logarithmic and power-law versions and pilgrim dark energy (PDE) models. Next, we introduce the (m,n) type pilgrim dark energy and its entropy-corrected versions of logarithmic and power-law forms i.e., (m,n) type LECPDE and PLECPDE models. The main motivation of the work is to have reconstructions of f(R), f(G), f(T), and Einstein-Aether gravities from (m,n) type entropy-corrected pilgrim dark energy (ECPDE). Briefly the idea of our proposed entropy-corrected (m,n) type pilgrim dark energy model is discussed. We also discuss the modified Friedmann equations for f(R), f(G), f(T), and Einstein-Aether gravities and then from the equations we find the effective density and pressure for the f(R), f(G), f(T), and Einstein-Aether gravities sectors, respectively. These can be treated as an effective dark energy. Assuming the power-law solution of the scale factor, a∼tδ, we can reconstruct the unknown functions of f(R), f(G), f(T), and F(K) of Einstein-Aether gravities from logarithmic and power-law corrected versions of ECPDE. Finally, we give some cosmological implications of the reconstructed models.

Reconstructing f(R) theory from pilgrim dark energy

We analyze pilgrim dark energy model in the background of f(R) gravity by taking IR cut-offs as particle and event horizons as well as conformal age of the universe. We regard the f(R) theory as an effective description for the pilgrim dark energy and reconstruct the function f(R) with the parameter μ<0 (which supports the phantom regime). Finally, we show the distinctive behavior of f(R) for the future cosmic evolution.

Pilgrim dark energy in f(T,T G ) cosmology

We work on the reconstruction scenario of pilgrim dark energy (PDE) in f(T,T G ). In PDE model it is assumed that a repulsive force that is accelerating the Universe is phantom type with (w DE <−1) and it is so strong that prevents formation of the black hole. We construct the f(T,T G ) models and correspondingly evaluate equation of state parameter for various choices of scale factor. Also, we assume polynomial form of f(T,T G ) in terms of cosmic time and reconstruct H and w DE in this manner. Through discussion, it is concluded that PDE shows aggressive phantom-like behavior for s=−2 in f(T,T G ) gravity.