Evolution of black hole shadow in the presence of ultralight bosons

Roy, Rittick; Yajnik, Urjit A.

doi:10.1016/j.physletb.2020.135284

Cited by 63 publications

(48 citation statements)

References 34 publications

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“…In particular, the shadows of a high-redshift supermassive black hole may serve as the standard rulers [22], which would constrain the cosmological parameters. Moreover, the EHT data may impose constraints in particle physics via the mechanism of superradiance [16,24,25].…”

Section: Introductionmentioning

confidence: 99%

Influence of quintessence dark energy on the shadow of black hole

2020

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We investigate the effects of quintessence dark energy on the shadows of black hole, surrounded by various profiles of accretions. For the thin-disk accretion, the images of the black hole comprises the dark region and bright region, including direct emission, lensing rings and photon rings. Although their details depend on the form of the emission, generically, direct emission plays a major role for the observed brightness of the black hole, while the lensing ring makes a small contribution and the photon ring makes a negligible contribution. The existence of a cosmological horizon also plays an important role in the shadows, since the observer in the domain of outer communications is near the cosmological horizon. For spherically symmetric accretion, static and infalling matters are considered. We find that the positions of photon spheres are the same for both static and infalling accretions. However, the observed specific intensity of the image for infalling accretion is darker than for static accretion, due to the Doppler effect of the infalling motion.

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Section: Introductionmentioning

confidence: 99%

Influence of quintessence dark energy on the shadow of black hole

2020

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“…The black hole companion for M87* can also be constrained through the image released by EHT [15]. Moreover, the information given by EHT can be used to impose constraints on particle physics via the mechanism of superradiance [16,17]. In particular, for the vector boson, it may constrain some of the fuzzy dark matter parameter space.…”

Section: Introductionmentioning

confidence: 99%

Shadows and photon spheres with spherical accretions in the four-dimensional Gauss–Bonnet black hole

2020

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We investigate the shadows and photon spheres of the four-dimensional Gauss–Bonnet black hole with the static and infalling spherical accretions. We show that, for both cases, there always exist shadows and photon spheres. The radii of the shadows and photon spheres are independent of the profiles of accretion for a fixed Gauss–Bonnet constant, implying that the shadow is a signature of the spacetime geometry and it is hardly influenced by accretion. Because of the Doppler effect, the shadows of the infalling accretion are found to be darker than in the static case. We also investigate the effect of the Gauss–Bonnet constant on the shadow and photon spheres, and we find that the larger the Gauss–Bonnet constant is, the smaller the radii of the shadow and photon spheres will be. In particular, the observed specific intensity increases as the Gauss–Bonnet constant grows.

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“…This means that the dynamical system of two kind of polarized photons is non-integrable and the shape of black hole shadow will change. Due to the equation (2.28) without separable variables, we must resort to "backward ray-tracing" method [43][44][45][46][47][48][49][50][51][52][53][54] to study numerically the shadow casted by such kinds of polarized lights. In this method, the light rays are assumed to evolve from the observer backward in time and the information carried by each ray would be respectively assigned to a pixel in a final image in the observer's sky.…”

Section: Kerr Black Hole Shadow Due To Coupling Between the Photon Anmentioning

confidence: 99%

“…where the transform matrix e ν µ obeys to γ µν e μ α e ν β = ηαβ, and ηαβ is the metric of Minkowski spactime. It is convenient to choose a decomposition associated with a reference frame with zero axial angular momentum in relation to spatial infinity [43][44][45][46][47][48][49][50][51][52][53][54][55][56]…”

Section: Kerr Black Hole Shadow Due To Coupling Between the Photon Anmentioning

confidence: 99%

“…Repeating the similar operations in refs. [43][44][45][46][47][48][49][50][51][52][53][54], one can obtain the position of photon's image in observer's sky 11) where the spatial position of observer is set to (r obs , θ obs ). In figures 2-5, we present black hole shadow for the different coupling constant α and rotation parameter a.…”

Section: Kerr Black Hole Shadow Due To Coupling Between the Photon Anmentioning

confidence: 99%

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Polarization effects in Kerr black hole shadow due to the coupling between photon and bumblebee field

Chen

Jing

2020

J. High Energ. Phys.

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We present firstly the equation of motion for the photon coupled to a special bumblebee vector field in a Kerr black hole spacetime and find that the propagation of light depends on its polarization due to the birefringence phenomenon. The dependence of black hole shadow on the light's polarization is dominated by the rotation of black hole. In the non-rotating case, we find that the black hole shadow is independent of the polarization of light. However, the status is changed in the rotating case, in which the black hole shadow depends on the light's polarization and the coupling between bumblebee vector field and electromagnetic field. These features of black hole shadow casted by polarized lights could help us to understand the bumblebee vector field with Lorentz symmetry breaking and its interaction with electromagnetic field.

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Evolution of black hole shadow in the presence of ultralight bosons

Cited by 63 publications

References 34 publications

Influence of quintessence dark energy on the shadow of black hole

Influence of quintessence dark energy on the shadow of black hole

Shadows and photon spheres with spherical accretions in the four-dimensional Gauss–Bonnet black hole

Polarization effects in Kerr black hole shadow due to the coupling between photon and bumblebee field

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