Exact model for a relativistic star

Tikekar, Ramesh

doi:10.1063/1.528851

Cited by 108 publications

(92 citation statements)

References 10 publications

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“…Some works also studied the viability of nonlinear EOS based on suitable geometry for the description in the interior 3-spaces of such compact star [11,86]. This approach leads to physically viable and easily tractable models of superdense stars in equilibrium.…”

Section: Introductionmentioning

confidence: 99%

Some new Wyman–Leibovitz–Adler type static relativistic charged anisotropic fluid spheres compatible to self-bound stellar modeling

Murad

Fatema

2015

Eur. Phys. J. C

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In this work some families of relativistic anisotropic charged fluid spheres have been obtained by solving the Einstein-Maxwell field equations with a preferred form of one of the metric potentials, and suitable forms of electric charge distribution and pressure anisotropy functions. The resulting equation of state (EOS) of the matter distribution has been obtained. Physical analysis shows that the relativistic stellar structure for the matter distribution considered in this work may reasonably model an electrically charged compact star whose energy density associated with the electric fields is on the same order of magnitude as the energy density of fluid matter itself (e.g., electrically charged bare strange stars). Furthermore these models permit a simple method of systematically fixing bounds on the maximum possible mass of cold compact electrically charged self-bound stars. It has been demonstrated, numerically, that the maximum compactness and mass increase in the presence of an electric field and anisotropic pressures. Based on the analytic models developed in this present work, the values of some relevant physical quantities have been calculated by assuming the estimated masses and radii of some well-known potential strange star candidates like PSR J1614-2230, PSR J1903+327, Vela X-1, and 4U 1820-30.

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Section: Introductionmentioning

confidence: 99%

Some new Wyman–Leibovitz–Adler type static relativistic charged anisotropic fluid spheres compatible to self-bound stellar modeling

Murad

Fatema

2015

Eur. Phys. J. C

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“…The Vaidya-Tikekar (VT) superdense stellar model incorporates a spheroidal geometry for the interior of the star [9]. The VT model has been shown to approximate the behaviour of neutron stars to a very good approximation [10].…”

Section: Introductionmentioning

confidence: 99%

A family of charged compact objects with anisotropic pressure

Maurya

Govender

2017

Eur. Phys. J. C

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Utilizing an ansatz developed by Maurya et al. we present a class of exact solutions of the Einstein-Maxwell field equations describing a spherically symmetric compact object. A detailed physical analysis of these solutions in terms of stability, compactness and regularity indicates that these solutions may be used to model strange star candidates. In particular, we model the strange star candidate Her X-1 and show that our solution conforms to observational data to an excellent degree of accuracy. An interesting and novel phenomenon which arises in this model is the fact that the relative difference between the electromagnetic force and the force due to the pressure anisotropy changing sign within the stellar interior. This may be an additional mechanism required for stability against cracking of the stellar object.

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“…It is now possible to write the solution of (16) explicitly as a series using the definitions of (17) and (18). With the help of (7) and (12) we obtain the expressions…”

Section: General Case : Series Solutionmentioning

confidence: 99%

“…Also Thirukkanesh and Maharaj [16] found a family of EinsteinMaxwell solutions that contain the Durgapal and Bannerji [17] neutron star model. [2] presented a general class of Einstein-Maxwell solutions that contain Tikekar [18] spheroidal stars as a special case which are physically viable neutron star models. Hence the approach followed in this paper has proved to be a fruitful avenue for generating new exact solutions for describing the interior spacetimes of charged spheres.…”

Section: Introductionmentioning

confidence: 99%

Classes of exact Einstein–Maxwell solutions

Komathiraj

Maharaj

2007

Gen Relativ Gravit

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We find new classes of exact solutions to the Einstein-Maxwell system of equations for a charged sphere with a particular choice of the electric field intensity and one of the gravitational potentials. The condition of pressure isotropy is reduced to a linear, second order differential equation which can be solved in general. Consequently we can find exact solutions to the Einstein-Maxwell field equations corresponding to a static spherically symmetric gravitational potential in terms of hypergeometric functions. It is possible to find exact solutions which can be written explicitly in terms of elementary functions, namely polynomials and product of polynomials and algebraic functions. Uncharged solutions are regainable with our choice of electric field intensity; in particular we generate the Einstein universe for particular parameter values.

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Exact model for a relativistic star

Cited by 108 publications

References 10 publications

Some new Wyman–Leibovitz–Adler type static relativistic charged anisotropic fluid spheres compatible to self-bound stellar modeling

Some new Wyman–Leibovitz–Adler type static relativistic charged anisotropic fluid spheres compatible to self-bound stellar modeling

A family of charged compact objects with anisotropic pressure

Classes of exact Einstein–Maxwell solutions

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