Strange star model with Tolmann IV type potential

Thirukkanesh, S.; Ragel, F. C.

doi:10.1007/s10509-014-1960-5

Cited by 39 publications

(28 citation statements)

References 45 publications

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“…[45,56,[67][68][69][70]82,95,99,100,102,105,106]. Models with such LEOS are discussed in [65,[93][94][95][96][97][98][99]. Obviously p r 0 = β (ρ 0 − ρ s ) > 0, p rs = 0.…”

Section: Solutions With Linear Eos and Simple Energy Densitymentioning

confidence: 99%

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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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“…[45,56,[67][68][69][70]82,95,99,100,102,105,106]. Models with such LEOS are discussed in [65,[93][94][95][96][97][98][99]. Obviously p r 0 = β (ρ 0 − ρ s ) > 0, p rs = 0.…”

Section: Solutions With Linear Eos and Simple Energy Densitymentioning

confidence: 99%

“…There are models with in addition given m, [93,94] or λ [95][96][97][98][99]. There are also models with quadratic EOS and λ [100][101][102].…”

Section: Introductionmentioning

confidence: 99%

Analytical study of anisotropic compact star models

Иванов

2017

Eur. Phys. J. C

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“…We observe that the function is regular if a > 0 A similar form of E can be used as shown by Tikekar et al, [5], Komathiraj et al, [3] and Islam S. et al, [2]. We consider the gravitational potential Z(r) [6] as,…”

Section: A Particular Class Of Solutionsmentioning

confidence: 84%

A parametric model to study the mass–radius relationship of stars

2019

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In static and spherically symmetric spacetime, we solve the Einstein Maxwell equations. The effective gravitational potential and the electric field for charged anisotropic fluid are defined in terms of two free parameters. For such configuration, the mass of the star as a function of stellar radius is found in terms of two aforementioned parameters, subjected to certain stability criteria. For various values of these two parameters one finds that such mass radius relationship can model stellar objects located at various regions of Hertzsprung-Russel diagram.

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“…The existence of anisotropy within a star can be explained by the presence of a solid core, phase transitions, a type III super fluid, a pion condensation [28] or another physical phenomenon by the presence of an electrical field [29]. Many researchers have used a great variety of mathematical techniques to try in order to obtain solutions of the Einstein-Maxwell field equations since it has been demonstrated by Komathiraj and Maharaj [30], Thirukkanesh and Maharaj [31], Maharaj et al [32], Thirukkanesh and Ragel [33,34], Feroze and Siddiqui [35,36], Sunzu et al [37], Pant et al [38] and Malaver [39][40][41][42]. These investigations show that the system of Einstein-Maxwell equations plays an important role to describe ultracompacts objects.…”

Section: Introductionmentioning

confidence: 99%

Analytical Models for Quark Stars with Van Der Waals Modified Equation of State

Malaver¹,

Kasmaei²

2019

IJASS

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Stellar models consisting of spherically symmetric distribution of charged matter locally anisotropic in strong gravitational fields have been widely considered in the frame of general relativity. These investigations require the generation of exact models through the resolution of the Einstein-Maxwell system of equations. The presence of charge produces values for redshifts, luminosity and mass for the stars different in relation to neutral matter. Some applications for dense charged matter we have them in the description of quark stars, spheres with linear or non-linear equation of state, hybrid stars and accreting process in compact objects where the matter acquires large amounts of electric charge. In this paper, we studied the behavior of relativistic compact objects with anisotropic matter distribution considering Van der Waals modified equation of state proposed in 2013 for Malaver and a gravitational potential Z(x) that depends on an adjustable parameter α in order to integrate analytically the field equations. They generalize the ideal gas law based on plausible reasons that real gases do not act ideally. New exact solutions of the Einstein-Maxwell system are generated and the physical variables as the energy density, radial pressure, mass function, anisotropy factor and the metric functions are written in terms of elementary and polynomial functions. We obtained expressions for radial pressure, density and mass of the stellar object physically acceptable with two different values of the adjustable parameter. The proposed models satisfy all physical features of a realistic star.

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Strange star model with Tolmann IV type potential

Cited by 39 publications

References 45 publications

Analytical study of anisotropic compact star models

Analytical study of anisotropic compact star models

A parametric model to study the mass–radius relationship of stars

Analytical Models for Quark Stars with Van Der Waals Modified Equation of State

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