Magnetized discs and photon rings around Yukawa-like black holes

Cruz-Osorio, Alejandro; Gimeno-Soler, Sergio; Font, José A.; De Laurentis, Mariafelicia; Mendoza, Sergio

doi:10.48550/arxiv.2102.10150

Cited by 5 publications

(5 citation statements)

References 66 publications

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“…In a number of interesting works, it is shown that the BH shadow can be investigated in interplay with other relevant ideas such as QNMs, deflection light and quasiperiodic oscillations (QPO) [102]- [112]. Additionally, it is known that the GTR-based magnetohydrodynamic simulations of the magnetized accretion flow onto BH can reveal more details of the BH shadow, see e.g [113][114][115][116].…”

Section: Introductionmentioning

confidence: 99%

No-hair theorem in the wake of Event Horizon Telescope

Khodadi

Lambiase²,

Mota³

2021

J. Cosmol. Astropart. Phys.

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Thanks to the release of the extraordinary EHT image of shadow attributed to the M87* supermassive black hole (SMBH), we have a novel window to assess the validity of fundamental physics in the strong-field regime. Motivated by this, we consider Johannsen & Psaltis metric parameterized by mass, spin, and an additional dimensionless hair parameter . This parametric framework in the high rotation regimes provides a well-behaved bed to the strong-gravity test of the no-hair theorem (NHT) using the EHT data. Incorporating the into the standard Kerr spacetime enrich it in the sense that, depending on setting the positive and negative values for that, we deal with alternative compact objects: deformed Kerr naked singularity and Kerr BH solutions, respectively. Shadows associated with these two possible solutions indicate that the deformation parameter affects the geometry shape of standard shadow such that it becomes more oblate and prolate with < 0 and > 0, respectively. By scanning the window associated with three shadow observables oblateness, deviation from circularity, and shadow diameter, we perform a numerical analysis within the range a * = 0.9 ∓ 0.1 of the dimensionless rotation parameter, to find the constraints on the hair parameter in both possible solutions. For both possible signs of , we extract a variety of upper bounds that are in interplay with a * . Although by approaching the rotation parameters to the extreme limit, the allowable range of both hair parameters becomes narrower, the hairy Kerr BH solution is a more promising candidate to play the role of the alternative compact object instead of the standard Kerr BH. The lack of tension between hairy Kerr BH with the current observation of the EHT shadow of the M87* SMBH carries this message that there is the possibility of NHT violation.

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Section: Introductionmentioning

confidence: 99%

No-hair theorem in the wake of Event Horizon Telescope

Khodadi

Lambiase²,

Mota³

2021

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

show abstract

“…In a number of interesting works, it is shown that the BH shadow can be investigated in interaction with other relevant ideas such as QNMs, deflection light and quasiperiodic oscillations (QPO) [102]- [112]. Additionally, it is believed that in the light of the GTR-based magnetohydrodynamic simulations of the magnetized accretion flows onto BH, thereby, more details of the BH shadow will become reveals for us, see e.g [113][114][115][116].…”

Section: Introductionmentioning

confidence: 99%

No-Hair Theorem in the Wake of Event Horizon Telescope

Khodadi,

Lambiase,

Mota

2021

Preprint

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Thanks to the release of the extraordinary EHT image of shadow attributed to the M87* supermassive black hole (SMBH), we have a novel window to assess the validity of fundamental physics in the strong-field regime. Motivated by this, we consider Johannsen & Psaltis metric parameterized by mass, spin and an additional dimensionless hair parameter which in the high rotation regimes is able to provide a suitable framework for the test of the no-hair theorem (NHT) using the EHT data. Incorporating the into the standard Kerr spacetime enrich it in the sense that, depending on setting the positive and negative values for that, we deal with alternative compact objects: deformed Kerr naked singularity and Kerr BH solutions, respectively. Shadows associated with these two possible solutions indicate that the deformation parameter affects the geometry shape of standard shadow such that it become more oblate and prolate with < 0 and > 0, respectively. By scanning the window associated with three shadow observables: oblateness, deviation from circularity, and shadow diameter, we perform a numerical analysis within the range a * = 0.9 ∓ 0.1 of the dimensionless rotation parameter, to find the constraints on the hair parameter in both possible solutions. For both possible signs of , we extract a variety of upper bounds that are in interplay with a * . Our analysis suggests that as the rotation parameter approaches the extreme limit, although the allowable range of both hair parameters becomes narrower, the hairy Kerr BH solution is a more promising candidate to play a role of the alternative compact object instead of standard Kerr BH. The lack of tension between hairy Kerr BH with the current observation of the EHT shadow of the M87* SMBH carries this message that the possibility of NHT violation is not excluded.

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“…Moreover, proofs of concept of the feasibility of testing general relativity, or even the existence of new particles via EHT observations have been reported in, e.g. [13][14][15][16][17][18][19].…”

Section: Introductionmentioning

confidence: 99%

Magnetized accretion disks around Kerr black holes with scalar hair: Constant angular momentum disks

et al. 2019

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Testing the true nature of black holes -the no-hair hypothesis -will become increasingly more precise in the next few years as new observational data is collected in both the gravitational wave channel and the electromagnetic channel. In this paper we consider numerically generated spacetimes of Kerr black holes with synchronised scalar hair and build stationary models of magnetized thick disks (or tori) around them. Our approach assumes that the disks are not self-gravitating, they obey a polytropic equation of state, the distribution of their specific angular momentum is constant, and they are marginally stable, i.e. the disks completely fill their Roche lobe. Moreover, contrary to existing approaches in the literature, our models are thermodinamically relativist, as the specific enthalpy of the fluid can adopt values significantly larger than unity. We study the dependence of the morphology and properties of the accretion tori on the type of black hole considered, from purely Kerr black holes with varying degrees of spin parameter, namely from a Schwarzschild black hole to a nearly extremal Kerr case, to Kerr black holes with scalar hair with different ADM mass and horizon angular velocity. Comparisons between the disk properties for both types of black holes are presented. The sequences of magnetized, equilibrium disks models discussed in this study can be used as initial data for numerical relativity codes to investigate their dynamical (non-linear) stability and used in tandem with ray-tracing codes to obtain synthetic images of black holes (i.e. shadows) in astrophysically relevant situations where the light source is provided by an emitting accretion disk.PACS numbers: 95.30. Sf, 04.70.Bw, 04.25.dg 95.30.Qd

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Magnetized discs and photon rings around Yukawa-like black holes

Cited by 5 publications

References 66 publications

No-hair theorem in the wake of Event Horizon Telescope

No-hair theorem in the wake of Event Horizon Telescope

No-Hair Theorem in the Wake of Event Horizon Telescope

Magnetized accretion disks around Kerr black holes with scalar hair: Constant angular momentum disks

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