Motion of massive particles around a charged Weyl black hole and the geodetic precession of orbiting gyroscopes

Fathi, Mohsen; Kariminezhad, Mona; Olivares, Manuel; Villanueva, J. R.

doi:10.1140/epjc/s10052-020-7945-3

Cited by 18 publications

(18 citation statements)

References 62 publications

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“…Accordingly, the lapse function (15) provides the exterior geometry of the CWBH. In the adopted geometric system of units, Q and λ have the dimensions of m. For λ > Q, this spacetime allows for two horizons; an event horizon r + , and a cosmological horizon r ++ (instead of a Cauchy horizon), given by [55] r…”

Section: The Black Hole Solutionmentioning

confidence: 99%

“…This solution is indeed the rotating counterpart of a particular static charged black hole, introduced in [52]. This charged Weyl black hole (CWBH) has been recently studied regarding the light propagation in vacuum and in plasmic medium [53,54] and the motion of neutral and charged particles [55,56]. As it is a rather interesting subject to understand how a black hole would appear in an observer's sky, it is therefore completely natural to discuss the optical properties of the rotating charged Weyl black hole (RCWBH) and its shadow.…”

Section: Introductionmentioning

confidence: 99%

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Ergosphere, Photon Region Structure, and the Shadow of a Rotating Charged Weyl Black Hole

2021

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In this paper, we explore the photon region and the shadow of the rotating counterpart of a static charged Weyl black hole, which has been previously discussed according to null and time-like geodesics. The rotating black hole shows strong sensitivity to the electric charge and the spin parameter, and its shadow changes from being oblate to being sharp by increasing in the spin parameter. Comparing the calculated vertical angular diameter of the shadow with that of M87*, we found that the latter may possess about 1036 protons as its source of electric charge, if it is a rotating charged Weyl black hole. A complete derivation of the ergosphere and the static limit is also presented.

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Section: The Black Hole Solutionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Ergosphere, Photon Region Structure, and the Shadow of a Rotating Charged Weyl Black Hole

2021

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“…In the case of our paper, we are in an even more extreme situation since we cannot provide an unambiguous physical interpretation to the parameter β because these analyses rely on the study of the geodesic motion which depends on the metric tensor and not the gravitational theory formulation. To our knowledge, this degeneracy has never been pointed out, despite the geodesic motion in the spacetime (1) has been extensively studied in the literature [25,[64][65][66][67][68][69][70][71][72][73][74][75][76][77][78][79][80][81][82][83].…”

Section: Physical Interpretation Of β: Accretion Disk and Shadowmentioning

confidence: 99%

“…H form > 4γ /3 assuming < 0 which constitutes a lower bound on the epoch of formation of the remnant. By using (68), an upper bound is set on the mass of the remnant as M r < 3/8. Restoring International System units by multiplying by c 2 /G, we get the bound on the remnant mass of M r < 0.5•10 27 kg, which is 1/4000 solar masses.…”

Section: Massive Gravitons or Anisotropic Fluid?mentioning

confidence: 99%

A critical assessment of black hole solutions with a linear term in their redshift function

2021

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Different theories of gravity can admit the same black hole solution, but the parameters usually have different physical interpretations. In this work we study in depth the linear term $$\beta r$$ β r in the redshift function of black holes, which arises in conformal gravity, de Rham–Gabadadze–Tolley (dRGT) massive gravity, f(R) gravity (as approximate solution) and general relativity. Geometrically we quantify the parameter $$\beta $$ β in terms of the curvature invariants. Astrophysically we found that $$\beta $$ β can be expressed in terms of the cosmological constant, the photon orbit radius and the innermost stable circular orbit (ISCO) radius. The metric degeneracy can be broken once black hole thermodynamics is taken into account. Notably, we show that under Hawking evaporation, different physical theories with the same black hole solution (at the level of the metric) can lead to black hole remnants with different values of their physical masses with direct consequences on their viability as dark matter candidates. In particular, the mass of the graviton in massive gravity can be expressed in terms of the cosmological constant and of the formation epoch of the remnant. Furthermore the upper bound of remnant mass can be estimated to be around $$0.5 \times 10^{27}$$ 0.5 × 10 27 kg.

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“…This black hole has also been recently examined in Refs. [30,31,32], regarding the behavior of null and time-like geodesics passing its exterior geometry, where the elliptic functions played an important role in the determination of the mass-less and (charged) massive particle trajectories. The shadow structure of a rotating counterpart of this black hole has been also discussed in Ref.…”

Section: Introductionmentioning

confidence: 99%

Роль Эллиптических Интегралов В Расчете Гравитационного Линзирования Заряженной Черной Дыры Вейля, Окруженной Плазмой

Fathi¹,

Villanueva²

2021

Вестник КРАУНЦ. Физико-Математические Науки

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In this paper, we mainly aim at highlighting the importance of (hyper-)elliptic integrals in the study of gravitational effects caused by strongly gravitating systems. For this, we study the application of elliptic integrals in calculating the light deflection as it passes a plasmic medium, surrounding a charged Weyl black hole. To proceed with this, we consider two specific algebraic ansatzes for the plasmic refractive index, and we characterize the photon sphere for each of the cases. This will be used further to calculate the angular diameter of the corresponding black hole shadow. We show that the complexity of the refractive index expressions, can result in substantially different types of dependencies of the light behavior on the spacetime parameters. В этой статье мы в основном стремимся подчеркнуть важность (гипер) эллиптических интегралов в изучении гравитационных эффектов, вызванных сильно гравитирующими системами. Для этого мы изучаем применение эллиптических интегралов при вычислении отклонения света при его прохождении через плазменную среду, окружающую заряженную черную дыру Вейля. Чтобы продолжить это, мы рассмотрим два конкретных алгебраических анзаца для показателя преломления плазмы и охарактеризуем фотонную сферу для каждого из случаев. Это будет использоваться в дальнейшем для вычисления углового диаметра соответствующей тени черной дыры. Мы показываем, что сложность выражений показателя преломления может привести к существенно разным типам зависимостей поведения света от пространственно-временных параметров.

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Motion of massive particles around a charged Weyl black hole and the geodetic precession of orbiting gyroscopes

Cited by 18 publications

References 62 publications

Ergosphere, Photon Region Structure, and the Shadow of a Rotating Charged Weyl Black Hole

Ergosphere, Photon Region Structure, and the Shadow of a Rotating Charged Weyl Black Hole

A critical assessment of black hole solutions with a linear term in their redshift function

Роль Эллиптических Интегралов В Расчете Гравитационного Линзирования Заряженной Черной Дыры Вейля, Окруженной Плазмой

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