Anisotropic stars made of exotic matter within the complexity factor formalism

Rincón, Ángel; Panotopoulos, Grigoris; Lopes, Ilídio

doi:10.1140/epjc/s10052-023-11262-y

Cited by 18 publications

(5 citation statements)

References 89 publications

(86 reference statements)

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“…Under this assumption, we can connect our solution smoothly by varying the parameters (including the isotropic pressure case) in a natural way. While a generalized Chaplygin equation of state has been used previously in the context of relativistic stars [48][49][50][51][52], the generalized double Chaplygin equation of state is a novel and unexplored approach that deserves considerable attention. Using these expressions, we can write the anisotropy factor (∆ = P ⊥ − P r ) as follows:…”

Section: The Generalized Double Chaplygin Modelmentioning

confidence: 99%

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A Generalized Double Chaplygin Model for Anisotropic Matter: The Newtonian Case

2023

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In this work, we investigate astrophysical systems in a Newtonian regime using anisotropic matter. For this purpose, we considered that both radial and tangential pressures satisfy a generalized Chaplygin-type equation of state. Using this model, we found the Lane–Emden equation for this system and solved it numerically for several sets of parameters. Finally, we explored the mass supported by this physical system and compared it with the Chandrasekhar mass.

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Section: The Generalized Double Chaplygin Modelmentioning

confidence: 99%

“…This behavior aligns with other solutions found in the context of compact stars and is logical considering that the second term in the anisotropic formula becomes more significant than the first term. For further insights and related references, refer to [52] and the cited sources therein.…”

Section: Casementioning

confidence: 99%

A Generalized Double Chaplygin Model for Anisotropic Matter: The Newtonian Case

2023

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“…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. It is apparent from the foregoing review of literature that physical possibilities of anisotropic stars are extensively explored by the researchers.…”

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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“…In this regard, some works on gravitational decoupling in the context of the complexity domain can be seen in the following Refs. [105][106][107][108][109][110][111].…”

Section: Introductionmentioning

confidence: 99%

Self-bound embedding Class I anisotropic stars by gravitational decoupling within vanishing complexity factor formalism

et al. 2023

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We present a spherically symmetric embedding Class I solution for compact star models using the gravitational decoupling approach. We have chosen a null complexity factor condition proposed by Herrera (Phys Rev D 97:044010, 2018) in the context of a self-gravitating system and derive the anisotropic solution through a systematic approach given by Contreras and Stuchlik (Eur Phys J C 82:706, 2022). In this regard, we use the Finch–Skea model along with the mimicking of mass constraint to find fluid pressure and the matter-energy density from the Einstein Field Equations (EFE). We tested the physical viability and impact of gravitational decoupling on the anisotropic solution through the graphical representation. Moreover, the energy exchange between the fluid distributions along with the mass-radius ratio of different compact objects has been also discussed.

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Anisotropic stars made of exotic matter within the complexity factor formalism

Cited by 18 publications

References 89 publications

A Generalized Double Chaplygin Model for Anisotropic Matter: The Newtonian Case

A Generalized Double Chaplygin Model for Anisotropic Matter: The Newtonian Case

Study of compact objects: a new analytical stellar model

Self-bound embedding Class I anisotropic stars by gravitational decoupling within vanishing complexity factor formalism

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