Static spherically symmetric wormholes in 
	    
	    
	   gravity*

Tayde, Moreshwar; Hassan, Zinnat; Sahoo, P. K.; Gutti, Sashideep

doi:10.1088/1674-1137/ac7f22

Cited by 41 publications

(16 citation statements)

References 78 publications

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“…Here α = 0 and β are free model parameters. The astrophysical implications of the considered model have been investigated in [35]. We are going to examine the cosmological behavior of the model.…”

Section: Model-iimentioning

confidence: 99%

“…Harko [30] argued that this dependence can be caused by exotic imperfect fluids or quantum phenomena. Recently, several cosmological and astrophysical aspects of f (Q, T ) gravity have been tested, for instance, Energy conditions [31], Baryogenesis [32], Cosmological inflation [33], Reconstruction of f (Q, T ) lagrangian [34], Static spherically symmetric wormholes [35], Constraint on the effective equation of state [36], Observational constraints on f (Q, T ) gravity models [37], and Cosmological perturbations [38]. However, except the introductory article, most other studies were primarily conducted to contact observational datasets and not much theoretical investigation was carried out in this gravity theory which is still at its infancy at best.…”

Section: Introductionmentioning

confidence: 99%

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f(Q, T) gravity, its covariant formulation, energy conservation and phase-space analysis

Loo

Solanki

et al. 2023

Eur. Phys. J. C

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In the present article we analyze the matter-geometry coupled f(Q, T) theory of gravity. We offer the fully covariant formulation of the theory, with which we construct the correct energy balance equation and employ it to conduct a dynamical system analysis in a spatially flat Friedmann–Lemaître–Robertson–Walker spacetime. We consider three different functional forms of the f(Q, T) function, specifically, $$f(Q,T)=\alpha Q+ \beta T$$ f ( Q , T ) = α Q + β T , $$f(Q,T)=\alpha Q+ \beta T^2$$ f ( Q , T ) = α Q + β T 2 , and $$f(Q,T)=Q+ \alpha Q^2+ \beta T$$ f ( Q , T ) = Q + α Q 2 + β T . We attempt to investigate the physical capabilities of these models to describe various cosmological epochs. We calculate Friedmann-like equations in each case and introduce some phase space variables to simplify the equations in more concise forms. We observe that the linear model $$f(Q,T)=\alpha Q+ \beta T$$ f ( Q , T ) = α Q + β T with $$\beta =0$$ β = 0 is completely equivalent to the GR case without cosmological constant $$\Lambda $$ Λ . Further, we find that the model $$f(Q,T)=\alpha Q+ \beta T^2$$ f ( Q , T ) = α Q + β T 2 with $$\beta \ne 0$$ β ≠ 0 successfully depicts the observed transition from decelerated phase to an accelerated phase of the universe. Lastly, we find that the model $$f(Q,T)= Q+ \alpha Q^2+ \beta T$$ f ( Q , T ) = Q + α Q 2 + β T with $$\alpha \ne 0$$ α ≠ 0 represents an accelerated de-Sitter epoch for the constraints $$\beta < -1$$ β < - 1 or $$ \beta \ge 0$$ β ≥ 0 .

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Section: Model-iimentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

f(Q, T) gravity, its covariant formulation, energy conservation and phase-space analysis

Loo

Solanki

et al. 2023

Eur. Phys. J. C

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“…While the creation of black holes is universal, requiring no unique matter composition, or energy condition (EC), the creation of wormholes is not as DOI: 10.1002/prop.202300197 straightforward or universal. [1] Wormholes are intriguing structures that link two distant points in spacetime. [2] Wormholes exhibit asymptotic flatness.…”

Section: Introductionmentioning

confidence: 99%

“…More values of 𝜐 DEC behave differently depending on the range of r. The SEC term 𝜌 +  r + 2 t violated the conditions as it behaves in a negative nature (see Figure14). Now for the range, 0 < 𝜐 ≤ 5, energy density behaves negatively in r ∈[1,4] (see Figure9). The NECs (seeFigures 10,11) disobey the scenario outside the throat radius.…”

mentioning

confidence: 96%

New Wormhole Solutions in Quadratic f(Q)$f(\mathcal {Q})$‐Gravity Regime

Kiroriwal,

Kumar,

Maurya

et al. 2024

Fortschritte der Physik

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Nowadays, alternative gravity is a crucial tool for addressing some enduring observational problems, such as the dark universe. Additionally, they can be used to advance the results of general relativity in astrophysics. Wormholes, or imagined passageways through spacetime, have the potential to revolutionize interstellar transport and cosmic interconnection. In the present work, the existence and characteristics of wormhole solutions in the context of the non‐linear function of gravity are investigated. A typical characteristic of maintaining wormholes is the presence of exotic stuff that defines the energy conditions (ECs). The authors looked at the ECs that must be met and analyzed how the function affects the energy‐momentum requirements for maintaining the wormholes open. For a comprehensive understanding of wormhole geometries, we also studied the embedding diagram and volume integral quantifier.

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“…In the context of

f(Q,T)

gravity, Tayde et al . [ 28 ] investigated the presence of spherically symmetric wormhole solutions under two intriguing non‐commutative geometries like the Gaussian and Lorentzian distributions of the string theory. The modified symmetric teleparallel gravity, or non‐metricity

f(Q)

gravity, which mimics the universe's background expansion, was the subject of a study by Mandal and Sahoo on observational constraints .…”

Section: Introductionmentioning

confidence: 99%

Singularity Free Star Model Characterized by Quintessence Field in Quadratic f(Q)$f(Q)$ Gravity

Bhar

2023

Fortschritte der Physik

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In the context of the theory of gravity, a spherically symmetric quintessence DE model in this article is offered. For this reason, has the formula , where Q stands for the non‐metricity scalar and ‘a’ is the coupling constant for modified gravity has been taken into account. It is supposed that the quintessence field defined by the parameter , where , controls the energy‐momentum tensor of the underlying fluid distribution. The relationship between several physical parameters for the selected values of ‘a’, by choosing the metric potentials suggested by the Krori‐Barua [Krori and Barua; J. Phys. A, Math. Gen. 8: 508, 1975] is investigated. Further, a number of analyses in detail to examine the physical validity of the proposed stellar model are carried out. The consequences of the compact star system caused by the connection of matter and geometry are succinctly described. The maximum allowable mass and radius for our present model for different values of ‘a’ have been studied by and curve. One can recover the usual general relativity (GR) standard results for .

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Static spherically symmetric wormholes in gravity*

Cited by 41 publications

References 78 publications

f(Q, T) gravity, its covariant formulation, energy conservation and phase-space analysis

f(Q, T) gravity, its covariant formulation, energy conservation and phase-space analysis

New Wormhole Solutions in Quadratic f(Q)$f(\mathcal {Q})$‐Gravity Regime

Singularity Free Star Model Characterized by Quintessence Field in Quadratic f(Q)$f(Q)$ Gravity

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