Radiating star with a time-dependent Karmarkar condition

Naidu, Nolene F.; Govender, M.

doi:10.1140/epjc/s10052-017-5457-6

Cited by 39 publications

(27 citation statements)

References 37 publications

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“…Finally, for the dynamic dissipative case, we recovered a known previous solution [31] and found a new shear-free Karmarkar radiating solution. 2 )r 2 )(βr 2 +1) n − 1 2 αr 2 (βr 2 +1))α (αr 2 +(βr 2 +1) n ) 2 (βr 2 +1)…”

Section: Final Remarkssupporting

confidence: 58%

“…• σ 1 = σ 2 , shear-free and a 1 = 0 geodesic fluids. Finally, considering shear-free and geodesic conditions in equations (23) y (24), we again obtain Y 1 = 0 3.5 The dissipative case: Z = 0 A recent paper [31] develops a model of a radiating relativistic sphere that satisfies the Karmarkar condition. It is the first dynamic dissipative model obtained.…”

Section: The Static Casementioning

confidence: 90%

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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: Final Remarkssupporting

confidence: 58%

Section: The Static Casementioning

confidence: 90%

Karmarkar scalar condition

Ospino

Núñez

2020

Eur. Phys. J. C

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“…In recent past, many attempts have been made by various authors to find exact analytic solutions of the Einstein field system using linear EOS with MIT bag model [25][26][27][28][29][30][31] as well as quadratic EOS [32][33][34][35][36][37][38][39]. On the other hand, various authors [40][41][42][43][44][45] have also explored new solutions of the Einstein field equations for anisotropic fluid under the Karmarkar condition [46].…”

Section: Introductionmentioning

confidence: 99%

Core-envelope model of super dense star with distinct equation of states

2019

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The aim of the present paper is to study an anisotropic spherically symmetric core-envelope model of a super dense star in which core is equipped with linear equation of state, consistent with the quark matter while the envelope is considered to be of quadratic equation of state by adopting the philosophy of Takisa et al. (Pramana J Phys 92:40, 2019). We demonstrate that all the physical parameters are realistic within the core as well as envelope of the stellar object and continuous at the junction. Our model is shown to be physically viable and substantiate with the strange stars SAX J1808.4-3658 and 4U1608-52. Further, We infer that if the mass of the star increases then central density results to higher values and core shrinks, which justifies the dominating effect of gravity for higher mass celestial objects.

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“…It is basically a mathematical tool which helps us in obtaining the exact solutions of field equations. In literature [89][90][91][92][93], this condition has been used by numerous researchers for discussing the compact stars models. In the present paper, we shall adopt the Karmarkar condition to develop the analytic solutions representing compact objects in f (R, T ) gravity.…”

Section: Introductionmentioning

confidence: 99%

Realistic stellar anisotropic model satisfying Karmarker condition in f(R, T) gravity

et al. 2020

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The present study explores the f (R, T) modified gravity on the basis of observational data for three different compact stars with matter profile as anisotropic fluid without electric charge. In this respect, we adopt the well-known Karmarker condition and assume a specific and interesting model for g rr metric potential component which is compatible with this condition. This choice further leads to a viable form of metric component g tt by utilizing the Karmarkar condition. We also present the interior geometry in the reference of Schwarzschild interior and Kohler-Chao cosmological like solutions for f (R, T) theory. Moreover, we calculate the spacetime constants by using the masses and radii from the observational data of three different compact stars namely 4U 1538-52, LMC X-4 and PSR J1614-2230. In order to explore the viability and stability of the obtained solutions, some physical parameters and properties are presented graphically for all three different compact object models. It is noticed that the parameters c and λ have some important and considerable role for these solutions. It is concluded that our obtained solutions are physically acceptable, bearing a well-behave nature in f (R, T) modified gravity.

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Radiating star with a time-dependent Karmarkar condition

Cited by 39 publications

References 37 publications

Karmarkar scalar condition

Karmarkar scalar condition

Core-envelope model of super dense star with distinct equation of states

Realistic stellar anisotropic model satisfying Karmarker condition in f(R, T) gravity

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