Anisotropic compact star with a linear pressure–density relationship

Das, Shyam; Parida, Bikram Keshari; Chakraborty, Koushik; Ray, Saibal

doi:10.1142/s0218271822500535

Cited by 9 publications

(4 citation statements)

References 68 publications

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“…Azmat and Zubair [29] considered Drugapal V solution for charged fluid sphere and extended it for anisotropic spherical distribution under the consideration of gravitational decoupling through Minimum Geometric Deformation. Das et al [30] in their model of anisotropic compact star found out the anisotropy function which is physically possible. They also calculated the tidal love number of the star.…”

Section: Introductionmentioning

confidence: 93%

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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Section: Introductionmentioning

confidence: 93%

Study of compact objects: a new analytical stellar model

Das,

Chakraborty,

Rahaman

et al. 2024

Eur. Phys. J. C

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“…[9][10][11][12][13][14][15] The impact of anisotropies in astrophysical and cosmological models have received widespread attention amongst researchers. [16][17][18][19][20][21][22][23][24][25][26][27][28][29][30][31][32][33] There exists a huge body of work on the effect of anisotropy on the evolution of temperature profiles during dissipative collapse by Govender and coworkers [34][35][36][37][38] and references therein. It has been shown that the presence of anisotropic pressures leads to higher temperatures at each interior point of the collapsing distribution with this effect being prominent in the central regions of the body.…”

Section: Introductionmentioning

confidence: 99%

Complexity‐Free Anisotropic Solution of Buchdahl's Model and Energy Exchange Between Relativistic Fluids by Extended Gravitational Decoupling

Maurya

Singh

Govender

et al. 2023

Fortschritte der Physik

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In this work, we present an anisotropic generalization of the Buchdahl static stellar model by implementing the method of extended gravitational decoupling and further requirement of vanishing complexity (Herrera, Phys Rev D 97:044010,2018). Starting off with a general spherically symmetric static metric with two unknown gravitational potentials, we impose the condition of vanishing complexity which then reduces the problem to a single-generating metric function [Contreras and Stuchlik, Eur. Phys. J. C (2022) 82:706]. The Buchdahl ansatz is then employed to obtain the complete gravitational behavior of the isotropic seed solution. The method of extended gravitational decoupling is thereafter utilized to obtain an anisotropic counterpart of the Buchdahl perfect gravitating sphere. We subject our solution to rigorous physical tests to ensure that it serves as a viable candidate for compact objects such as neutron stars as well as pulsars. We show that the decoupling parameter plays a crucial role in determining the stability and regularity of several key physical features of the entire stellar model. A novel finding of our investigation is the energy exchange between the seed solution and the secondary source which we show is sensitive to the decoupling parameter. In addition, it has also been shown that the direction of energy flow depends on the radial distance of the shell from the center of the stellar configuration.

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“…Bhar and collaborators investigated an anisotropic solution in Tolman spacetime [45] and in 2 + 1 dimensions in Finch-Skea spacetime [46]. Some of the recent work on anisotropic compact stars and cosmological modeling can be found in [47][48][49][50][51][52][53][54][55][56][57][58][59][60][61][62][63].…”

Section: Introductionmentioning

confidence: 99%

Anisotropic compact stellar solution in general relativity

et al. 2023

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We present herein a new class of singularity-free interior solutions to describe realistic anisotropic compact stellar objects with spherically symmetric matter distribution. A specific form of anisotropy is assumed to obtain the exact solution for the field equation. Smooth matching of interior solutions thus obtained with the Schwarzschild exterior metric over the bounding surface of a compact star, together with the condition that the radial pressure vanishes at the boundary, is used to obtain the mathematical form for the model parameters. The pulsar 4U1608-52 with its current estimated data (mass $$=1.57 ~M\odot $$ = 1.57 M ⊙ and radius $$=9.8 \pm 0.8$$ = 9.8 ± 0.8 km; Özel et al. in ApJ 820:28, 2016) is used to study the model graphically.

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Anisotropic compact star with a linear pressure–density relationship

Cited by 9 publications

References 68 publications

Study of compact objects: a new analytical stellar model

Study of compact objects: a new analytical stellar model

Complexity‐Free Anisotropic Solution of Buchdahl's Model and Energy Exchange Between Relativistic Fluids by Extended Gravitational Decoupling

Anisotropic compact stellar solution in general relativity

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