No-hair theorem in the wake of Event Horizon Telescope

Abstract

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.

Testing Horndeski Gravity from EHT Observational Results for Rotating Black Holes

“…While the first-order correction to the circular shadow shape occurs due to the spin in Kerr spacetime, in MoGs the distortion for a given spin may arise due to other hairs (Cunha et al 2015(Cunha et al , 2019Afrin et al 2021;Ghosh et al 2021;Khodadi et al 2021)-this prompts the use of shadow observables for the determination of black hole parameters (Hioki & Maeda 2009;Afrin et al 2021;Afrin & Ghosh 2022). It has been shown in multiple studies that observables like the shadow radius R s and distortion δ s (Hioki & Maeda 2009) demand some specific symmetry in the shadow shape, and thus they may not be efficient in some MoGs (Tsukamoto et al 2014;Abdujabbarov et al 2015;).…”

Parameterizations of black-hole spacetimes beyond circularity

“…Conversely, the circular spacetimes in [68], based on the parameterization [13], can feature a dent in the shadow boundary, but no cusps.…”

Weak Gravitational Lensing in Dark Matter and Plasma Mediums for Wormhole-like Static Aether Solution

“…In this section, let us examine the photonsphere and the shadow produced by the wormhole considered in this study. There have been various studies of the shadow of black holes and shadow of wormholes [31,32,[62][63][64][65][66][67][68][69][70][71][72][73][74][75][76][77][78][79][80][81]. But first time here we will include the influence of a non-magnetized cold plasma with plasma frequency ω p (r), which can be done through by means of deriving the equations of motion (EoS) through the Hamiltonian [45] to wormhole spacetime.…”