Anisotropic compact stars with Karmarkar condition in energy-momentum squared gravity

Sharif, M.; Gul, M. Zeeshan

doi:10.1007/s10714-022-03062-8

Cited by 22 publications

(4 citation statements)

References 86 publications

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“…[ 48 ] It has been observed that CSs are not physically viable and stable at the center in

f(\mathcal {R},\mathcal {T}^{2})

theory. [ 49 ] Here, we have found that all the considered CSs are physically viable and stable in this modified theory.…”

Section: Final Remarksmentioning

confidence: 69%

Viable and Stable Compact Stellar Structures in f(Q,T)$f(\mathcal {Q},\mathcal {T})$ Theory

Gul,

Sharif,

Arooj

2024

Fortschritte der Physik

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The main objective of this paper is to investigate the impact of gravity on the geometry of anisotropic compact stellar objects, where is non‐metricity and is the trace of the energy‐momentum tensor. In this perspective, the physically viable non‐singular solutions to examine the configuration of static spherically symmetric structures is used. A specific model of this theory to examine various physical quantities in the interior of the proposed compact stars (CSs) is considered. These quantities include fluid parameters, anisotropy, energy constraints, equation of state parameters, mass, compactness, and redshift. The Tolman–Oppenheimer–Volkoff equation is used to examine the equilibrium state of stellar models, while the stability of the proposed CSs is investigated through sound speed and adiabatic index methods. It is found that the proposed CSs are viable and stable in the context of this theory.

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“…[ 48 ] It has been observed that CSs are not physically viable and stable at the center in

f(\mathcal {R},\mathcal {T}^{2})

theory. [ 49 ] Here, we have found that all the considered CSs are physically viable and stable in this modified theory.…”

Section: Final Remarksmentioning

confidence: 69%

Viable and Stable Compact Stellar Structures in f(Q,T)$f(\mathcal {Q},\mathcal {T})$ Theory

Gul,

Sharif,

Arooj

2024

Fortschritte der Physik

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“…In the realm of f (R) theory, the results indicate the instability of the Her X-1 compact star associated with the second gravity model due to the limited range satisfied by the physical quantities [96]. Furthermore, in the framework of f (R, T 2 ) theory, it is found that compact stars are neither physically viable nor stable at the center [97]. In light of these findings, it can be concluded that all considered compact stars exhibit both physical viability and stability in this modified theory.…”

Section: Final Remarksmentioning

confidence: 93%

Study of viable compact stellar structures in non-Riemannian geometry

Gul,

Sharif,

Arooj

2024

Phys. Scr.

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The main objective of this article is to investigate the viablecompact stellar structures in non-Riemannian geometry, i.e.,$f(\mathbb{Q},\mathbb{T})$ theory, where $\mathbb{Q}$ defines thenon-metricity and $\mathbb{T}$ represents trace of the stress-energytensor. For this purpose, we consider a static spherical spacetimewith anisotropic matter configuration to examine the geometry ofconsidered compact stars. A specific model of this theory is used toderive the explicit expressions of energy density and pressurecomponents that govern the relationship between matter and geometry.The unknown constants in the metric potentials are determined byusing the continuity of interior and exterior spacetimes to examinethe configuration of spherical stellar structures. Physicalparameters such as fluid characteristics, energy constraints andequation of state parameters are analyzed to examine the viabilityof the considered stellar objects. Further, the equilibrium stateand stability of the proposed stellar objects are evaluated usingthe Tolman-Oppenheimer-Volkoff equation, sound speed and adiabaticindex, respectively. The rigorous analysis and satisfaction ofnecessary conditions lead to the conclusion that the stellar objectsstudied in this framework are viable and stable.

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“…We have analyzed the viability and stability of compact stars with different matter distributions in f (, 𝕋 2 ) theory. [49] Recently, Yousaf et al [50] investigated the impact of a newly developed modified f (, 𝕋 2 ) theory on the complexity of time-dependent dissipative/non-dissipative spherically symmetric celestial structures with and without charge.…”

Section: Doi: 101002/prop202200184mentioning

confidence: 99%

Study of Charged Anisotropic Karmarkar Stars in f(R,T2)$f(\mathcal {R},\mathbb {T}^{2})$ Theory

Sharif

Gul

2023

Fortschritte der Physik

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This paper examines the viable attributes of charged compact stars with anisotropic matter configuration in ffalse(scriptR,T2false)$f(\mathcal {R},\mathbb {T}^{2})$ theory. For this purpose, we use the embedding class‐1 technique and consider a specific functional form of this modified theory, i.e, f(R,double-struckT2)=scriptR−γT2$f(\mathcal {R},\mathbb {T} ^{2})=\mathcal {R}-\gamma \mathbb {T}^{2}$ to examine the geometry of compact objects. The values of unknown parameters are found by the smooth matching of interior (static spherical metric) and exterior (Reissner‐Nordstrom metric of energy‐momentum squared gravity) spacetimes. We investigate the impact of effective fluid parameters anisotropy, equation of state parameters and energy bounds in the inner region of the charged stellar objects. The stability of the stellar models in the presence of charge is examined by speed of sound and adiabatic index. We find that embedding class‐1 solution is physically viable and stable for charged anisotropic stellar objects in this modified theory.

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Anisotropic compact stars with Karmarkar condition in energy-momentum squared gravity

Cited by 22 publications

References 86 publications

Viable and Stable Compact Stellar Structures in f(Q,T)$f(\mathcal {Q},\mathcal {T})$ Theory

Viable and Stable Compact Stellar Structures in f(Q,T)$f(\mathcal {Q},\mathcal {T})$ Theory

Study of viable compact stellar structures in non-Riemannian geometry

Study of Charged Anisotropic Karmarkar Stars in f(R,T2)$f(\mathcal {R},\mathbb {T}^{2})$ Theory

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