Stationary axially symmetric Brans-Dicke-Maxwell fields

Singh, T.; N., L.

doi:10.1007/bf00756670

Cited by 19 publications

(17 citation statements)

References 21 publications

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“…( 12) to find ν. Hereafter, we will employ a more direct method, yielding the solutions readily from known GR solutions, up to possible coordinate transformation. Actually, as we have discussed in the Introduction, there is such a method in the literature, given in [23,24], which successfully generated many BD(-Maxwell) solutions from the known solutions of GR theory. In the next subsection, a more general form of this method, containing one extra parameter apart from the BD parameter ω, will be presented, with the help of the Ernst equations obtained in the above analysis.…”

Section: A Spacetime and Field Equationsmentioning

confidence: 99%

“…Besides these methods, following the earlier works on this subject [18][19][20][21][22], an identification technique is presented by Nayak and Tiwari [23] for axially symmetric vacuum solutions and generalized for Maxwell vacuum fields by Sing and Rai [24]. The main idea of this method is to employ a standard stationary, axially symmetric spacetime metric and the field variables sharing the symmetries of this metric and compare the field equations of both theories to find some transformations to reduce the field equations of BD theory to those of GR.…”

Section: Introductionmentioning

confidence: 99%

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Stationary axially symmetric solutions in Brans-Dicke theory

Kirezli

Delice

2015

Phys. Rev. D

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Stationary, axially symmetric Brans-Dicke-Maxwell solutions are reexamined in the framework of the Brans-Dicke (BD) theory. We see that, employing a particular parametrization of the standard axially symmetric metric simplifies the procedure of obtaining the Ernst equations for axially symmetric electrovacuum space-times for this theory. This analysis also permits us to construct a two parameter extension in both Jordan and Einstein frames of an old solution generating technique frequently used to construct axially symmetric solutions for BD theory from a seed solution of general relativity. As applications of this technique, several known and new solutions are constructed including a general axially symmetric BD-Maxwell solution of Plebanski-Demianski with vanishing cosmological constant, i.e. the Kinnersley solution and general magnetized Kerr-Newman-type solutions. Some physical properties and the circular motion of test particles for a particular subclass of Kinnersley solution, i.e., a Kerr-Newman-NUT-type solution for BD theory, are also investigated in some detail.Brans-Dicke (BD) scalar-tensor theory [1] is the most studied alternative theory of gravity generalizing general relativity (GR) in a consistent way by introducing a scalar field replacing Newton's gravitational constant. Being one of the most straightforward extension of GR, this theory draws a lot of interest and helps to test various aspects of GR. The peculiar differences were noted in the exact solutions of this theory compared to the similar solutions of GR. For example, static spherically symmetric vacuum solutions of BD theory [2], unlike GR, do not describe asymptotically flat black holes [3] resulting from gravitational collapse, unless the scalar field becomes a constant. This is due to the fact that corresponding solutions in BD theory cannot meet three important criteria, namely, asymptotic flatness, regularity at the horizon and the weak energy condition, simultaneously. After the discovery of spherically and axially symmetric exact solutions, it was realized that there are ranges of parameters in which these solutions describe black holes [4][5][6][7][8] where the first two criteria are met but the third one is not. However, these ranges are at the nonphysical negative values of the BD parameter, ω, where the kinetic term becomes negative. Hence, it is concluded that the black holes of BD theory obeying these three conditions must be the same as the black holes of GR, requiring a constant BD scalar. Although they are the same, their perturbations can behave differently [9] owing to the fact that they are the solutions of different theories. Thus, the differences between perturbations of GR and BD theories for the same black hole solution might be another tool [9,10] to test BD theory against GR.Obtaining exact solutions of any theory is important for several reasons, such as, for comparisons with observational results or for obtaining the outcomes of the theory under consideration. One important class of these solutions with a grea...

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Section: A Spacetime and Field Equationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Stationary axially symmetric solutions in Brans-Dicke theory

Kirezli

Delice

2015

Phys. Rev. D

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“…Bruckman and Kazes [42] evaluated the form of scalar field corresponding to perfect fluid. Singh and Rai [43] presented a method to formulate stationary axially symmetric solutions of BD Maxwell field equations. Demiański-type metric was obtained through a complex coordinate transformation by Krori and Bhattacharjee [44].…”

Section: Introductionmentioning

confidence: 99%

Decoupled Embedding Class-One Strange Stars in Self-Interacting Brans–Dicke Gravity

Sharif

Majid

2021

Universe

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This work aims to extend two isotropic solutions to the anisotropic domain by decoupling the field equations in self-interacting Brans–Dicke theory. The extended solutions are obtained by incorporating an additional source in the isotropic fluid distribution. We deform the radial metric potential to disintegrate the system of field equations into two sets such that each set corresponds to only one source (either isotropic or additional). The system related to the anisotropic source is solved by employing the MIT bag model as an equation of state. Further, we develop two isotropic solutions by plugging well-behaved radial metric potentials in Karmarkar’s embedding condition. The junction conditions at the surface of the star are imposed to specify the unknown constants appearing in the solution. We examine different physical characteristics of the constructed quark star models by using the mass and radius of PSR J1903+327. It is concluded that, in the presence of a massive scalar field, both stellar structures are well-behaved, viable and stable for smaller values of the decoupling parameter.

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“…Obtaining Ernst BD equations is one of the most known of these techniques [12][13][14]. Also, Nayak and Tiwari [15] obtained vacuum stationary, axially symmetric BD solutions and generalized Maxwell field by Rai and Singh [16]. Their theory depends on finding out the relation between the field equations of BD and GR theories.…”

Section: Introductionmentioning

confidence: 99%

Brans-Dicke Solutions of Stationary, Axially Symmetric Spacetimes

Uludağ¹

2020

Advances on Tensor Analysis and Their Applications

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One of the most known alternative gravitational theories is Brans-Dicke (BD) theory. The theory offers a new approach by taking a scalar field ϕ instead of Newton's gravitational constant G. Solutions of the theory are under consideration and results are discussed in many papers. Stationary, axially symmetric solutions become important because gravitational field of celestial objects can be described by such solutions. Since obtaining exact solutions of BD is not an easy task, some solution-generating techniques are proposed. In this context, some solutions of Einstein general relativity, such as black hole or wormhole solutions, are discussed in BD theory. Indeed, black hole solutions in BD theory are not fully understood yet. Old and new such solutions and their analysis will be reviewed in this chapter.

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Stationary axially symmetric Brans-Dicke-Maxwell fields

Cited by 19 publications

References 21 publications

Stationary axially symmetric solutions in Brans-Dicke theory

Stationary axially symmetric solutions in Brans-Dicke theory

Decoupled Embedding Class-One Strange Stars in Self-Interacting Brans–Dicke Gravity

Brans-Dicke Solutions of Stationary, Axially Symmetric Spacetimes

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