Anisotropic fluid spheres admitting Karmarkar condition in <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" altimg="si8.svg"><mml:mrow><mml:mi>f</mml:mi><mml:mo>(</mml:mo><mml:mi mathvariant="script">G</mml:mi><mml:mo>,</mml:mo><mml:mi mathvariant="bold-script">T</mml:mi><mml:mo>)</mml:mo></mml:mrow></mml:math> gravity

Mustafa, Ghulam; Shamir, M. Farasat; Ahmad, M.; Ashraf, Asifa

doi:10.1016/j.cjph.2020.07.017

Cited by 37 publications

(5 citation statements)

References 46 publications

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“…The anisotropic solutions of the internal compact structure is developed by using the radial and temporal metric components given in Eq. (39). Some new constraints can be employed to determine the solution of Eqs.…”

Section: Gravitational Decoupling Via Mgdmentioning

confidence: 99%

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Influence of charge on decoupled anisotropic spheres in f(G, T) gravity

Sharif

Hassan

2022

Eur. Phys. J. Plus

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In this paper, we develop two anisotropic solutions for static selfgravitating spherical structure in the presence of electromagnetic field through gravitational decoupling approach in f (G, T ) theory, where G and T denote the Gauss-Bonnet term and trace of the energymomentum tensor, respectively. The extra source with isotropic seed sector is responsible for generating anisotropy in the spacetime. The system of field equations is decoupled into two arrays by using minimal geometric deformation in the radial component. The first set portrays the isotropic regime whereas the second set represents the anisotropic system. The metric coefficients of the Krori-Barua spacetime are employed to extract solution of the first set while two constraints on the radial and temporal components of the extra source yield the corresponding two solutions. Finally, we investigate the influence of charge and decoupling parameter on the physical viability and stability of the obtained solutions. We conclude that the resulting solutions in this modified theory indicate more feasible and stable structures.

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Section: Gravitational Decoupling Via Mgdmentioning

confidence: 99%

“…For the effectiveness of the stellar matter source, both the EoS parameters (radial and tangential) must lie in [0,1] [39].…”

Section: Solution IImentioning

confidence: 99%

Influence of charge on decoupled anisotropic spheres in f(G, T) gravity

Sharif

Hassan

2022

Eur. Phys. J. Plus

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“…The solutions conform to all the conditions of physical viability. Anisotropic solutions are studied in other modified theories of gravity [33][34][35]. Rincón et al [36] studied the role of complexity factor on the physical features of anisotropic stars considering a generalized Chaplygin equation of state.…”

Section: Introductionmentioning

confidence: 99%

Study of compact objects: a new analytical stellar model

Das,

Chakraborty,

Rahaman

et al. 2024

Eur. Phys. J. C

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In this paper, we obtain analytical solutions of Einstein field equations for a spherically symmetric anisotropic matter distributions. For this purpose physically meaningful metric potential corresponds to $$g_{rr}$$ g rr and a particular choice of the anisotropy has been utilized to obtain the solutions in closed form. This class of solution has been used to characterized observed pulsars from different aspects. Smooth matching of interior spacetime metric with the exterior Schwarzschild metric and in addition with the condition of vanishing radial pressure across the boundary leads us to determine the model parameters. Pulsar $$4U1820-30$$ 4 U 1820 - 30 with its current estimated data for mass and radius (Mass $$=1.58 M_\odot $$ = 1.58 M ⊙ and radius $$=9.1$$ = 9.1 km) has been allowed for testing the physical acceptability of our developed model. We have graphically analyzed the gross physical features of the observed pulsar. The stability of the model is also discussed under the conditions of causality, adiabatic index and generalized Tolman–Oppenheimer–Volkov (TOV) equation under the forces acting on the system. Few more pulsars with their have been considered, to show that this model is compatible with observational data, and all the requirements of a realistic star are highlighted. Mass-radius (M–R) relationship have been generated for our model. The impact of anisotropy on the gross physical features of stars have been explored with the graphical presentation.

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“…We have discussed the dynamics of gravitational collapse with different matter distributions in the same theory [48]. Mustafa et al [49] analyzed anisotropic fluid spheres admitting Karmarkar condition in this gravity. Maurya et al [50] studied the possible existence of anisotropic spherically symmetric solutions in the arena of modified  ( ) f , T theory.…”

Section: Introductionmentioning

confidence: 99%

Role of f(\mathcal{R},\mathbf{T}^{2}) Theory on Charged Compact Stars

Sharif

Gul²

2023

Phys. Scr.

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The main purpose of this paper is to examine the viable attributes of charged compact stellar objects with anisotropic matter configuration in the framework of $f(\mathcal{R},\mathbf{T}^{2})$ theory. For this purpose, we use Tolman V solution and consider a specific functional form of this modified theory to examine the geometry of compact stars. The values of unknown parameters are found by the smooth matching of interior (static spherical metric) and exterior (modified Reissner-Nordstrom metric) spacetimes. We investigate the behavior of effective matter variables, anisotropy, equation of state parameters and energy bounds in the interior of the charged stellar objects. The stability of the compact stars is examined by speed of sound and adiabatic index. We find that the considered stars are viable as well as stable with all the required conditions in this modified theory of gravity.

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Anisotropic fluid spheres admitting Karmarkar condition in f(G,T) gravity

Cited by 37 publications

References 46 publications

Influence of charge on decoupled anisotropic spheres in f(G, T) gravity

Influence of charge on decoupled anisotropic spheres in f(G, T) gravity

Study of compact objects: a new analytical stellar model

Role of f(\mathcal{R},\mathbf{T}^{2}) Theory on Charged Compact Stars

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