Erratum to: Black hole solution and strong gravitational lensing in Eddington-inspired Born–Infeld gravity

Wei, Shao-Wen; Yang, Ke; Liu, Yu-Xiao

doi:10.1140/epjc/s10052-015-3556-9

Cited by 46 publications

(28 citation statements)

References 3 publications

(3 reference statements)

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“…An approximate form of this result for null rays was obtained by Bozza in Ref. [8] and used/re-derived by many others in particular spacetimes [11][12][13][14][15][16][17][18][19][20]38]. When n → ∞, θ ∞,s becomes independent of C 0 , D 0 as well as φ sd and reaches its minimal value, i.e., the size of the black hole shadow…”

Section: Gl and Bh Shadow Size In The Sflmentioning

confidence: 69%

“…Previously, GL in the strong field limit in other spacetimes has been studied extensively using traditional GL equations (see e.g. [20,46]). While for Hayward spacetime, Ref.…”

Section: The Hayward Bh Spacetime Casementioning

confidence: 99%

“…The existence of photon sphere (surface) around some BHs [5] has been well known, and the location of the innermost stable circular orbits [6,7] has been intensively investigated. In particular, the deflection of null rays in the SFL has been systematically studied by Bozza et al for static and spherically symmetric (SSS) spacetimes and equatorial motion in stationary and axisymmetric (SAS) spacetimes [8][9][10] and has since been used to study the deflection and GL in the SFL for many interesting spacetimes [11][12][13][14][15][16][17][18][19][20][21]. Note that most of the deflection angles found in these works assumed that the source and detectors are located at infinite distance.…”

Section: Introductionmentioning

confidence: 99%

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Perturbative deflection angle, gravitational lensing in the strong field limit and the black hole shadow

Jia

Huang

2021

Eur. Phys. J. C

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A perturbative method to compute the deflection angle of both timelike and null rays in arbitrary static and spherically symmetric spacetimes in the strong field limit is proposed. The result takes a quasi-series form of $$(1-b_c/b)$$ ( 1 - b c / b ) where b is the impact parameter and $$b_c$$ b c is its critical value, with coefficients of the series explicitly given. This result also naturally takes into account the finite distance effect of both the source and detector, and allows to solve the apparent angles of the relativistic images in a more precise way. From this, the BH angular shadow size is expressed as a simple formula containing metric functions and particle/photon sphere radius. The magnification of the relativistic images were shown to diverge at different values of the source-detector angular coordinate difference, depending on the relation between the source and detector distance from the lens. To verify all these results, we then applied them to the Hayward BH spacetime, concentrating on the effects of its charge parameter l and the asymptotic velocity v of the signal. The BH shadow size were found to decrease slightly as l increases to its critical value, and increase as v decreases from light speed. For the deflection angle and the magnification of the images however, both the increase of l and decrease of v will increase their values.

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Section: Gl and Bh Shadow Size In The Sflmentioning

confidence: 69%

“…Previously, GL in the strong field limit in other spacetimes has been studied extensively using traditional GL equations (see e.g. [20,46]). While for Hayward spacetime, Ref.…”

Section: The Hayward Bh Spacetime Casementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Perturbative deflection angle, gravitational lensing in the strong field limit and the black hole shadow

Jia

Huang

2021

Eur. Phys. J. C

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“…Another way to solve the problems is to modify the theory of gravity and these modified theories can generate interesting astrophysical and cosmological consequences [53]. Strong field gravitational lensings can provide a possible way to test and distinguish theoretical predictions in the vicinity of a compact body by these modified theories of gravity and GR [54][55][56][57][58][59][60][61][62][63][64][65][66][67][68][69][70][71][72]. In this work, we will study the string field lensing in the SDL by a charged Galileon black hole.…”

Section: Introductionmentioning

confidence: 99%

Strong field gravitational lensing by a charged Galileon black hole

Zhao

Xie

2016

J. Cosmol. Astropart. Phys.

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Strong field gravitational lensings are dramatically disparate from those in the weak field by representing relativistic images due to light winds one to infinity loops around a lens before escaping. We study such a lensing caused by a charged Galileon black hole, which is expected to have possibility to evade no-hair theorem. We calculate the angular separations and time delays between different relativistic images of the charged Galileon black hole. All these observables can potentially be used to discriminate a charged Galileon black hole from others. We estimate the magnitudes of these observables for the closest supermassive black hole Sgr A*. The strong field lensing observables of the charged Galileon black hole can be close to those of a tidal Reissner-Nordström black hole or those of a Reissner-Nordström black hole. It will be helpful to distinguish these black holes if we can separate the outermost relativistic images and determine their angular separation, brightness difference and time delay, although it requires techniques beyond the current limit.

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“…Although, this theory is completely equivalent to Einstein's general relativity in vacuum, significant deviations from general relativity manifest themselves if the energy density or its space-time gradients are sufficiently large [7][8][9][10][11][12][13][14]. This is particularly true in the extreme environments attained in the early universe [15][16][17][18][19][20][21][22][23] and inside black holes [24][25][26][27][28][29][30][31][32][33], which may, if certain conditions are verified, be singularity free (see, however, [34][35][36][37][38]). …”

Section: Introductionmentioning

confidence: 99%

Mass inflation in Eddington-inspired Born-Infeld black holes: Analytical scaling solutions

Avelino

2016

Phys. Rev. D

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We study the inner dynamics of accreting Eddington-inspired Born-Infeld black holes using the homogeneous approximation and taking charge as a surrogate for angular momentum. We show that there is a minimum of the accretion rate below which mass inflation does not occur, and we derive an analytical expression for this threshold as a function of the fundamental scale of the theory, the accretion rate, the mass, and the charge of the black hole. Our result explicitly demonstrates that, no matter how close Eddington-inspired Born-Infeld gravity is to general relativity, there is always a minimum accretion rate below which there is no mass inflation. For larger accretion rates, mass inflation takes place inside the black hole as in general relativity until the extremely rapid density variations bring it to an abrupt end. We derive analytical scaling solutions for the value of the energy density and of the Misner-Sharp mass attained at the end of mass inflation as a function of fundamental scale of the theory, the accretion rate, the mass, and the charge of the black hole, and compare these with the corresponding numerical solutions. We find that, except for unreasonably high accretion rates, our analytical results appear to provide an accurate description of homogeneous mass inflation inside accreting Eddington-inspired Born-Infeld black holes.

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Erratum to: Black hole solution and strong gravitational lensing in Eddington-inspired Born–Infeld gravity

Cited by 46 publications

References 3 publications

Perturbative deflection angle, gravitational lensing in the strong field limit and the black hole shadow

Perturbative deflection angle, gravitational lensing in the strong field limit and the black hole shadow

Strong field gravitational lensing by a charged Galileon black hole

Mass inflation in Eddington-inspired Born-Infeld black holes: Analytical scaling solutions

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