Constructing black holes in Einstein–Maxwell-scalar theory

Yu, Shuang; Qiu, Jianhui; Gao, Changjun

doi:10.1088/1361-6382/abf2f5

Cited by 19 publications

(11 citation statements)

References 79 publications

(61 reference statements)

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“…The above study fully illustrates the motivations for the novel Einstein Maxwell-scalar theory S 3 [35][36][37], as well as the connection between it and the dilaton model. Now, let us extend our grasp of this theory by considering rotation, starting with the associated static solution of S 3 , and concentrating on the search for a slowly rotating black hole solution in asymptotically flat spacetime.…”

Section: Action and The Equations Of Motionmentioning

confidence: 66%

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Slowly rotating black holes in the novel Einstein–Maxwell-scalar theory

Qiu

2021

Eur. Phys. J. C

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We investigate a slowly rotating black hole solution in a novel Einstein–Maxwell-scalar theory, which is prompted by the classification of general Einstein–Maxwell-scalar theory. The gyromagnetic ratio of this black hole is calculated, and it increases as the second free parameter $$\beta $$ β increases, but decreases with the increasing parameter $$\gamma \equiv \frac{2 \alpha ^{2}}{1+\alpha ^2}$$ γ ≡ 2 α 2 1 + α 2 . In the Einstein–Maxwell-dilaton (EMD) theory, the parameter $$\beta $$ β vanishes but the free parameter $$\alpha $$ α governing the strength of the coupling between the dilaton and the Maxwell field remains. The gyromagnetic ratio is always less than 2, the well-known value for a Kerr–Newman (KN) black hole as well as for a Dirac electron. Scalar hairs reduce the magnetic dipole moment in dilaton theory, resulting in a drop in the gyromagnetic ratio. However, we find that the gyromagnetic ratio of two can be realized in this Einstein–Maxwell-scalar theory by increasing $$\beta $$ β and the charge-to-mass ratio Q/M simultaneously (recall that the gyromagnetic ratio of KN black holes is independent of Q/M). The same situation also applies to the angular velocity of a locally non-rotating observer. Moreover, we analyze the period correction for circular orbits in terms of charge-to-mass ratio, as well as the correction of the radius of the innermost stable circular orbits. It is found the correction increases with $$\beta $$ β but decreases with Q/M. Finally, the total radiative efficiency is investigated, and it can vanish once the effect of rotation is considered.

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Section: Action and The Equations Of Motionmentioning

confidence: 66%

“…Turimov et al [36] have investigated the geodesic of this theory. We extended it by combining RN BHs and general dilaton BHs [35] and by considering higher dimensions [37]. The present article is devoted to the study of the slowly rotating black hole in four-dimensional and asymptotically flat spacetime.…”

Section: Introductionmentioning

confidence: 99%

Slowly rotating black holes in the novel Einstein–Maxwell-scalar theory

Qiu

2021

Eur. Phys. J. C

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“…From the theoretical and observational studies, the existence of an accretion disk around black holes is expected to be the primary source of information about gravity and geometry in the strong field regime. It can also enable very potent tests for probing unknown aspects of high energy phenomena occurring in the close vicinity of black holes [61]. Therefore, it has value to consider important and valuable insights of the spacetime geometry in the strong field regime that can have a significant impact on the test particle geodesics and can result in changing observable quantities, that is, the innermost stable circular orbit (ISCO) and accretion disk parameters.…”

Section: Introductionmentioning

confidence: 99%

Radiation properties of the accretion disk around a black hole in Einstein-Maxwell-scalar theory*

Alloqulov,

Shaymatov,

Ahmedov

et al. 2024

Chinese Phys. C

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In this paper, we investigate the luminosity of the accretion disk of a black hole in Einstein-Maxwell-scalar (EMS) theory. We determine all orbital parameters of particles in the accretion disk, e.g., angular velocity, angular momentum, energy, and radius of the innermost circular stable orbit (ISCO). Further, we analyze the flux, differential luminosity and temperature of the accretion disk. Finally, we study the radiative efficiency for different values of black hole parameters.

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“…This theory has proven to support several black hole configurations with different asymptotic geometries. To give some examples, asymptotically AdS and Lifshitz black hole solutions within Einstein-Maxwell-scalar theories with different coupling functions and self-interaction scalar potentials are presented in [22] and [23], respectively. Meanwhile spherical black holes in Einstein-Maxwell-scalar models where the scalar field is coupled to the Maxwell invariant are discussed in [24].…”

Section: Introductionmentioning

confidence: 99%

Hyperscaling violating Schrodinger black holes in Einstein-Maxwell-scalar theory

Herrera-Aguilar,

Paschalis,

Romero-Figueroa

2021

Preprint

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We present a novel family of asymptotically Schrödinger hyperscaling violating black holes with a generic dynamical critical exponent z and an arbitrary number of spacetime dimensions. This black hole family represents a solution within the Einstein-Maxwell-scalar setup with a self-interaction scalar potential where the Maxwell field is coupled to the scalar field. Through an analysis of the curvature invariants it is observed that this configuration is asymptotically regular for different ranges of the hyperscaling violating exponent θ. Furthermore, the above mentioned solution constitutes a gravitational candidate for describing field theories with hyperscaling violating Schrödinger symmetry at finite temperature within the framework of the Gravity/Condensed Matter Theory correspondence.

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Constructing black holes in Einstein–Maxwell-scalar theory

Cited by 19 publications

References 79 publications

Slowly rotating black holes in the novel Einstein–Maxwell-scalar theory

Slowly rotating black holes in the novel Einstein–Maxwell-scalar theory

Radiation properties of the accretion disk around a black hole in Einstein-Maxwell-scalar theory*

Hyperscaling violating Schrodinger black holes in Einstein-Maxwell-scalar theory

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