Pilgrim Dark Energy Parameter Research Articles

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.

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.

Cosmological analysis of reconstructed {mathcal {F}}(T,T_{mathcal {G}}) models

In this paper, we analyze cosmological consequences of the reconstructed generalized ghost pilgrim dark energy {mathcal {F}}(T,T_{mathcal {G}}) models in terms of redshift parameter z. For this purpose, we consider power-law scale factor, scale factor for two unified phases and intermediate scale factor. We discuss graphical behavior of the reconstructed models and examine their stability analysis. Also, we explore the behavior of equation of state as well as deceleration parameters and omega _{Lambda }-omega _{Lambda }^{'} as well as r-s planes. It is found that all models are stable for pilgrim dark energy parameter 2. The equation of state parameter satisfies the necessary condition for pilgrim dark energy phenomenon for all scale factors. All other cosmological parameters show great consistency with the current behavior of the universe.

Pilgrim dark energy models in fractal universe

We discuss the cosmological implications of interacting pilgrim dark energy (PDE) models (with Hubble, Granda–Oliveros and generalized ghost cutoffs) with cold dark matter ([Formula: see text]CDM) in fractal cosmology by assuming the flat universe. We observe that the Hubble parameter lies within observational suggested ranges while deceleration parameter represents the accelerated expansion behavior of the universe. The equation of state (EoS) parameter ([Formula: see text]) corresponds to the quintessence region and phantom region for different cases of [Formula: see text]. Further, we can see that [Formula: see text]–[Formula: see text] (where prime indicates the derivative with respect to natural logarithmic of scale factor) plane describes the freezing and thawing regions and also corresponds to [Formula: see text] limit for some cases of [Formula: see text] (PDE parameter). It is also noted that the [Formula: see text]–[Formula: see text] (state-finder parameters) plane corresponds to [Formula: see text] limit and also shows the Chaplygin as well as phantom/quintessence behavior. It is observed that pilgrim dark energy models in fractal cosmology expressed the consistent behavior with recent observational schemes.

Anisotropic Generalized Ghost Pilgrim Dark Energy Model in General Relativity

A spatially homogeneous and anisotropic locally rotationally symmetric (LRS) Bianchi type-I Universe filled with matter and generalized ghost pilgrim dark energy (GGPDE) has been studied in general theory of relativity. To obtain determinate solution of the field equations we have used scalar expansion proportional to the shear scalar which leads to a relation between the metric potentials. Some well-known cosmological parameters (equation of state (EoS) parameter (ωΛ), deceleration parameter (q) and squared speed of sound \({v_{s}^{2}}\)) and planes (\(\omega _{\Lambda }-\dot {\omega }_{\Lambda }\) and statefinder) are constructed for obtained model. The discussion and significance of these parameters is totally done through pilgrim dark energy parameter (β) and cosmic time (t).

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.

Some Bianchi type generalized ghost piligrim dark energy models in general relativity

In this paper, we consider Bianchi type- $\mathit{III}$ , $V$ and $\mathit{VI}_{0}$ space-times filled with generalized ghost pilgrim dark energy (GGPDE) in general relativity. Here we assume the anisotropic distribution of GGPDE by introducing skewness parameters. To get deterministic solutions, we consider the scale factor $a(t)=(t^{n}e^{t})^{ \frac{1}{k}}$ , so called hybrid expansion, which yields a time dependent deceleration parameter, and exhibits a transition of the Universe from early decelerated phase to the recent accelerating phase. To describe the behavior of the obtained models we construct equation of state ( $\omega_{\varLambda }$ ), squared sound speed ( $v_{s}^{2}$ ) parameters and $\omega_{\varLambda }$ – $\dot{\omega }_{\varLambda }$ , $r$ – $s$ planes. It is worth mentioning here that the analysis of evolution parameters supports the concept of pilgrim dark energy (PDE). Also, these models remain stable for PDE parameter $\beta =-0.5$ . Moreover, the cosmological planes correspond to $\varLambda \mathit{CDM}$ limit as well as different well-known dark energy models.

Cosmological evolution of generalized ghost pilgrim dark energy in f ( T ) $f(T)$ gravity

We explore the phenomenon that phantom-like dark energy prevents the formation of black holes by assuming the generalized ghost version of pilgrim dark energy in the background of generalized teleparallel gravity. In this scenario, we construct \(f(T)\) model for explaining the evolutionary behavior of equation of state parameter, \(\omega_{\varLambda}-\omega'_{\varLambda}\) and \(r-s\) planes. We discuss these cosmological parameters graphically by taking different values of redshift parameter and pilgrim dark energy parameter. It is found that the equation of state parameter shows phantom like behavior while \(\omega_{\varLambda}-\omega'_{\varLambda}\) plane possesses thawing region for some particular values of pilgrim dark energy parameter. The statefinder parameters in \(r-s\) plane indicate the behavior of quintessence and phantom models. Finally, we discuss the first and second laws of thermodynamics and investigate the behavior of entropy production term.

Cosmological analysis of pilgrim dark energy in loop quantum cosmology

The proposal of pilgrim dark energy is based on speculation that phantom-like dark energy (with strong enough resistive force) can prevent black hole formation in the universe. We explore this phenomenon in loop quantum cosmology framework by taking Hubble horizon as an infra-red cutoff in pilgrim dark energy. We evaluate the cosmological parameters such as Hubble, equation of state parameter, squared speed of sound and also cosmological planes like $\omega_{\vartheta}-\omega'_{\vartheta}$ and $r-s$ on the basis of pilgrim dark energy parameter ($u$) and interacting parameter ($d^2$). It is found that values of Hubble parameter lies in the range $74^{+0.005}_{-0.005}$. It is mentioned here that equation state parameter lies within the ranges $-1\mp0.00005$ for $u=2, 1$ and $(-1.12,-1), (-5,-1)$ for $u=-1,-2$, respectively. Also, $\omega_{\vartheta}-\omega'_{\vartheta}$ planes provide $\Lambda$CDM limit, freezing and thawing regions for all cases of $u$. It is also interesting to mention here that $\omega_{\vartheta}-\omega'_{\vartheta}$ planes lie in the range ($\omega_{\vartheta}=-1.13^{+0.24}_{-0.25}, \omega'_{\vartheta}<1.32$). In addition, $r-s$ planes also corresponds to $\Lambda$CDM for all cases of $u$. Finally, it is remarked that all the above constraints of cosmological parameters shows consistency with different observational data like Planck, WP, BAO, $H_0$ and SNLS.

Cosmological Evolution of Pilgrim Dark Energy inf(G)Gravity

We analyze the behavior of pilgrim dark energy with Hubble horizon inf(G)gravity. We reconstruct thef(G)models through correspondence phenomenon by assuming two values of pilgrim dark energy parameter(u=2, -2). We evaluate the equation of state parameter which shows evolution of the universe in the quintessence, vacuum, and phantom phase for both cases ofuand give favor the pilgrim dark energy phenomenon. Also, squared speed of sound exhibits the stability off(G)model for both cases ofu. ThewPDE-wPDE′also provides freezing and thawing regions in this scenario. In this framework, ther-splane also corresponds to different dark energy scenarios.

Analysis of generalized ghost pilgrim dark energy in non-flat FRW universe

This work is based on pilgrim dark energy conjecture which states that phantom-like dark energy possesses the enough resistive force to preclude the formation of black hole. The non-flat geometry is considered which contains the interacting generalized ghost pilgrim dark energy with cold dark matter. Some well-known cosmological parameters (evolution parameter ($\omega_{\Lambda}$) and squared speed of sound) and planes ($\omega_{\Lambda}$-$\omega_{\Lambda}'$ and statefinder) are constructed in this scenario. The discussion of these parameters is totally done through pilgrim dark energy parameter ($u$) and interacting parameter ($d^2$). It is interesting to mention here that the analysis of evolution parameter supports the conjecture of pilgrim dark energy. Also, this model remains stable against small perturbation in most of the cases of $u$ and $d^2$. Further, the cosmological planes correspond to $\Lambda$CDM limit as well as different well-known dark energy models.

Pilgrim dark energy with apparent and event horizons in non-flat universe

Pilgrim dark energy is an interesting proposal which is based on the conjecture that phantom-like dark energy with strong enough repulsive force can prevent the formation of a black hole. We investigate this conjecture by assuming the apparent and event horizons in non-flat universe and we develop different cosmological parameters. We construct the corresponding equation of state parameter, which indicates that its present values lie in the phantom era of the universe for different ranges of μ (pilgrim dark energy parameter) as well as ξ2 (interacting parameter). It is interesting to mention here that the pilgrim dark energy with event horizon yields a phantom region for all cases of ξ2 with μ<0. We also develop the ωΛ–\(\omega'_{\varLambda}\) plane and explore the thawing as well as freezing region and ΛCDM limit for these models. The statefinders plane is also constructed, which shows the correspondence with different models such as quintessence and phantom dark energy, ΛCDM and Chaplygin gas. Finally, we investigate the validity of the generalized second law of thermodynamics with event horizon in a flat as well as non-flat universe.