Anisotropic stars for spherically symmetric spacetimes satisfying the Karmarkar condition

Maurya, S. K.; Ratanpal, B. S.; Govender, M.

doi:10.1016/j.aop.2017.04.008

Cited by 68 publications

(32 citation statements)

References 35 publications

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“…As shown in figure 1 Karmarkar's condition has experimented a recent boom, with more than 70 publications in the last three years, most of them devoted in describing anisotropic compact objects. There are many interesting models of possible compact objects, depending on the variety of the metric function selected as input: rational functions [6,7,8,9,10,11,12], polynomials [13,14,15,16,17], trigonometric [18,19,20,21] and hyperbolic functions [22,23,24]. Recently, there have been some explorations of the consequences of the Karmarkar conditions on stellar structure models in modified theories of gravity [25,26].…”

Section: Introductionmentioning

confidence: 99%

Karmarkar scalar condition

Ospino

Núñez

2020

Eur. Phys. J. C

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In this work we present the Karmarkar condition in terms of the structure scalars obtained from the orthogonal decomposition of the Riemann tensor. This the new expression becomes an algebraic relation among the physical variables, and not a differential equation between the metric coefficients. By using the Karmarkar scalar condition we implement a method to obtain all possible embedding class I static spherical solutions, provided the energy density profile is given. We also analyse the dynamic adiabatic case and show the incompatibility of the Kamarkar condition with several commonly assumed simplifications to the study of gravitational collapse. Finally, we consider the dissipative dynamic Karmarkar collapse and find a new solution family.

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Section: Introductionmentioning

confidence: 99%

Karmarkar scalar condition

Ospino

Núñez

2020

Eur. Phys. J. C

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“…However, the solutions resulting from the two theories are completely different. In Karmarkar spacetime there are no physical solutions describing isotropic fluid distributions, however, physical solution exist if electric charge or anisotropy or both are incorporated [28][29][30][31][32][33][34][35][36][37][38][39][40][41][42]. In this article also we are exploring new physical solutions satisfying field equations under class I category and discuss the solutions to model compact stars.…”

Section: Introductionmentioning

confidence: 99%

Compact star models in class I spacetime

et al. 2019

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In the present article, we have presented completely new exact, finite and regular class I solutions of Einstein's field equations i.e. the solutions satisfy the K armarkar condition. For this purpose needfully we have introduced a completely new suitable g rr metric potential to generate the model. We have investigated the various physical aspects for our model such as energy density, pressure, anisotropy, energy conditions, equilibrium, stability, mass, surface and gravitational red-shifts, compactness parameter and their graphical representations. All these physical aspects have ensured that our proposed solutions are wellbehaved and hence represent physically acceptable models for anisotropic fluid spheres. The models have satisfied causality and energy conditions. The presented models are also stable by satisfying Bondi condition and Abreu et al. condition, in equilibrium position and static by satisfying TOV equation, Harrison-Zeldovich-Novikov condition, respectively. For the parameters chosen in the paper are matching in modeling Vela X-1, Cen X-3, EXO 1785-248 and LMC X-4. The M-R graph generated from the solutions is matching the ranges of masses and radii for the considered compact stars. This work also estimated the approximate moment of inertia for the mentioned compact stars.

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“…(43) and (51), while the radial speed of sound satisfies the sufficient condition Eq. (36). Equation (61) …”

Section: Tangential Pressure and The Main Pair Of Inequalitiesmentioning

confidence: 99%

“…In some of them the generating metric component is a polynomial [23][24][25][26][27][28], in others it is a rational function [29][30][31]. There are also trigonometric [32,33], hyperbolic [34] and exponential generating metric components [35,36].…”

Section: Introductionmentioning

confidence: 99%

Analytical study of anisotropic compact star models

Иванов

2017

Eur. Phys. J. C

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A simple classification is given of the anisotropic relativistic star models, resembling the one of charged isotropic solutions. On the ground of this database, and taking into account the conditions for physically realistic star models, a method is proposed for generating all such solutions. It is based on the energy density and the radial pressure as seeding functions. Numerous relations between the realistic conditions are found and the need for a graphic proof is reduced just to one pair of inequalities. This general formalism is illustrated with an example of a class of solutions with linear equation of state and simple energy density. It is found that the solutions depend on three free constants and concrete examples are given. Some other popular models are studied with the same method.

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Anisotropic stars for spherically symmetric spacetimes satisfying the Karmarkar condition

Cited by 68 publications

References 35 publications

Karmarkar scalar condition

Karmarkar scalar condition

Compact star models in class I spacetime

Analytical study of anisotropic compact star models

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