A revisit of rotating black hole shadow with astrometric observables

Chang, Zhe; Zhu, Qing-Hua

doi:10.48550/arxiv.2001.05175

Cited by 6 publications

(6 citation statements)

References 33 publications

(62 reference statements)

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“…V. RADIUS OF THE SHADOW analysis of shapes of the black hole shadows have been recently considered in a great number of papers (see, for example, [7][8][9][10][11][12][13][14] and references therein). The radius of the photon sphere r ph of a spherically symmetric black hole is determined by means of the following function: (see, for example, [37,38] and references therein)…”

Section: B the (In)stability Regionmentioning

confidence: 99%

Quasinormal modes, stability and shadows of a black hole in the 4D Einstein-Gauss-Bonnet gravity

Konoplya,

Zinhailo

2020

Preprint

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Recently a non-trivial (3 + 1)-dimensional Einstein-Gauss-Bonnet theory of gravity was formulated in [D. Glavan and C. Lin, Phys. Rev. Lett. 124, 081301 (2020)] which bypasses the Lovelock's theorem and avoids Ostrogradsky instability. Here we calculate quasinormal modes of scalar, electromagnetic and gravitational perturbations and find the radius of shadow for spherically symmetric and asymptotically flat black holes in this theory. We show that, when the coupling constant is positive, the black hole is gravitationally unstable unless α is small enough (0 < α 0.15). At the same time, the negative coupling constant allows for a stable black-hole solution up to relatively large absolute values of α (0 > α −2.0). The instability is the eikonal one. It develops in the both, axial and polar, channels of gravitational perturbations at high multipole numbers. The radius of the shadow R Sh obeys the linear law R Sh ≈ (3 √ 3/2) + 0.94α with a remarkable accuracy.

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Section: B the (In)stability Regionmentioning

confidence: 99%

Quasinormal modes, stability and shadows of a black hole in the 4D Einstein-Gauss-Bonnet gravity

Konoplya,

Zinhailo

2020

Preprint

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“…While the literature on the study of shadow cast is quite exhaustive before and after the release of the black hole image by the EHT, it leaves no doubt about the importance of studying the black hole shadow since it reveals imprints of the spacetime being considered, and the effects of any type of astrophysical environments . It led to various methods being developed to explore such effects [60][61][62][63][64][65][66][67][68]. This study aims to constrain the screening factor γ using the EHT data and explore how the shadow cast/radius behaves.…”

Section: Introductionmentioning

confidence: 99%

Shadow, lensing, quasinormal modes, greybody bounds and neutrino propagation by dyonic ModMax black holes

et al. 2022

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Motivated by recent work on the Modified Maxwell (ModMax) black holes [Phys Lett B 10.1016/j.physletb.2020.136011], which are invariant in duality rotations and conformal transformations founded in [Phys Rev D 10.1103/PhysRevD.102.121703], we probe its effects on the shadow cast, weak field gravitational lensing, and neutrino propagation in its vicinity. Using the EHT data for the shadow diameter of Sgr. A* and M87*, and LIGO/VIRGO experiments for the dyonic ModMax black hole perturbations, we find constraints for ModMax parameters such as $$Q_\text {m}$$ Q m and the screening factor $$\gamma $$ γ . We also analyze how the shadow radius behaves as perceived by a static observer and one that is comoving with the cosmic expansion. The effect of the ModMax parameters is constant for a static observer, and we found That it varies when the observer is comoving with cosmic expansion. We also analyzed its effect on the weak deflection angle by exploiting the Gauss–Bonnet theorem and its application to Einstein ring formation. We also consider the finite distance effect and massive particle deflection. Our results indicate that the far approximation of massive particle gives the largest deflection angle and amplifies the effect of $$Q_\text {m}$$ Q m and $$\gamma $$ γ . Then we also calculate the quasinormal modes and greybody bounds which encode unique characteristic features of the dyonic ModMax black hole. With the advent of improving space technology, we reported that it is possible to detect the deviation caused through the shadow cast, Einstein rings, quasinormal modes, and neutrino oscillations.

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“…1 In addition, the optical appearance of a star orbiting a black hole is also an interesting topic to study, see examples in [22][23][24][25][26][27][28][29][30][31]. Furthermore, the shadow of a black hole observed by other physical observers also has people's attention, some interesting results can be found in [32][33][34][35].…”

Section: Null Geodesic In Quantum Corrected Schwarzschild Black Holementioning

confidence: 99%

Influence of Quantum Correction on the Black Hole Shadows, Photon Rings and Lensing Rings

Peng,

Guo,

Feng

2020

Preprint

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We calculate the photon sphere r ph and critical curve b c for the quantum corrected Schwarzschild black hole, finding that they violate an universal inequalities proved for asymptotically flat black holes which satisfy null energy condition in the framework of Einstein gravity. This violation seem to be a common phenomenon when considering quantum modification of Einstein gravity. Furthermore, we study the shadows, lensing rings and photon rings in the quantum corrected Schwarzschild black hole. The violation leads to a larger bright lensing ring in the observational appearance of thin disk emission near the black hole compared with the classical Schwarzschild black hole. Our analysis may provide a observational evidence for quantum effect of general relativity.

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A revisit of rotating black hole shadow with astrometric observables

Cited by 6 publications

References 33 publications

Quasinormal modes, stability and shadows of a black hole in the 4D Einstein-Gauss-Bonnet gravity

Quasinormal modes, stability and shadows of a black hole in the 4D Einstein-Gauss-Bonnet gravity

Shadow, lensing, quasinormal modes, greybody bounds and neutrino propagation by dyonic ModMax black holes

Influence of Quantum Correction on the Black Hole Shadows, Photon Rings and Lensing Rings

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