Shadows of rotating wormholes

Shaikh, Rajibul

doi:10.1103/physrevd.98.024044

Cited by 196 publications

(150 citation statements)

References 100 publications

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“…However, due to an improper estimation of the wormhole mass, the contribution of the light ring at the throat to the shadow boundary is overestimated, resulting in much rounder images. In addition, as a result of the same inaccuracy, the wormhole images reported in [41] are bigger, approaching the shadow of the Kerr black hole in size. .…”

Section: Wormhole Shadowsmentioning

confidence: 97%

“…The influence of the wormhole throat on its shadow was investigated previously in [41]. However, due to an improper estimation of the wormhole mass, the contribution of the light ring at the throat to the shadow boundary is overestimated, resulting in much rounder images.…”

Section: Wormhole Shadowsmentioning

confidence: 99%

“…In this case the metric function g rr vanishes, and the trajectories are determined by the conditions They lead to the implicit relation between the celestial coordinates α and β [41] …”

Section: Rotating Traversable Wormholesmentioning

confidence: 99%

“…An analytical expression for the shadow boundary associated with the outer spherical orbits was obtained previously in [2], but the shadow analysis presented there was incomplete. A second work [41] derived the shadow rim resulting from the spherical orbits at the throat and presented the wormhole images as a superposition of the two boundary curves. Unfortunately, due to improper estimation of the wormhole mass, the shadow images reported in [41] deviate from the realistic ones both qualitatively and in terms of scale.…”

Section: Introductionmentioning

confidence: 99%

“…A second work [41] derived the shadow rim resulting from the spherical orbits at the throat and presented the wormhole images as a superposition of the two boundary curves. Unfortunately, due to improper estimation of the wormhole mass, the shadow images reported in [41] deviate from the realistic ones both qualitatively and in terms of scale. Therefore, we revisit the problem by summarizing current results, and by computing the wormhole shadows both analytically by means of the boundary curves and numerically using a ray-tracing program.…”

Section: Introductionmentioning

confidence: 99%

See 4 more Smart Citations

On the shadow of rotating traversable wormholes

et al. 2018

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We revisit the shadow of rotating traversable wormholes discussing the role of the wormhole throat in the shadow formation. For certain classes of wormholes the throat serves as a potential barrier for light rays with particular impact parameters, thus modifying the shadow shape. We consider a couple of wormhole solutions and examine the structure of their shadow images, and the intrinsic mechanisms for their formation. Some of the shadows possess cuspy edges, which arise due to the interplay of two distinct families of unstable spherical orbits. These solutions provide examples, in which the explicit mechanism for cusp formation can be uncovered.

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Section: Wormhole Shadowsmentioning

confidence: 97%

Section: Wormhole Shadowsmentioning

confidence: 99%

“…In this case the metric function g rr vanishes, and the trajectories are determined by the conditions They lead to the implicit relation between the celestial coordinates α and β [41] …”

Section: Rotating Traversable Wormholesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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On the shadow of rotating traversable wormholes

et al. 2018

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Quasinormal Modes of Static Ellis-Bronnikov Wormholes

Azad

2023

Lecture Notes in Physics

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Quasinormal modes represent characteristic features of compact objects, since they entail their reaction to perturbations. While black holes and neutron stars in general relativity have been extensively studied and their quasinormal modes are well-known, the complete set of quasinormal modes for wormholes was only recently obtained. Here we discuss how to determine these quasinormal modes of Ellis-Bronnikov wormholes. These wormholes are static spherically symmetric solutions of general relativity coupled to a phantom scalar field. We obtain the axial and polar quasinormal modes and show, that for the massless wormhole a threefold degeneracy of the modes arises, i.e., there is isospectrality of the modes.

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Shadows and Accretion Disk Images of Compact Objects

Nedkova

2023

Lecture Notes in Physics

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The black hole shadow was predicted theoretically already in the 1960s as a strong gravitational lensing phenomenon. Recently, its observation became feasible and opened a major experimental channel for probing the gravitational interaction in the strong field regime. Although considered historically as a property of the black hole spacetimes, the shadow is not exclusively a black hole effect and does not require the presence of an event horizon. Other compact objects can also cast a shadow if their gravitational field is sufficiently strong bringing up the issue of how we can differentiate between self-gravitating systems based on their shadow images. In this chapter we discuss the analytical or semi-analytical methods for obtaining the observable images produced by compact objects in some basic physical settings such as a uniform spherical distribution of distant light sources or the presence of a thin accretion disk. We review the calculation of the shadow boundary for the Kerr black hole and focus on recent research on the images created by wormholes and naked singularities. These compact objects can look qualitatively very similar to black holes in some cases, but they can also possess clear-cut observational signatures.

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Shadows of rotating wormholes

Cited by 196 publications

References 100 publications

On the shadow of rotating traversable wormholes

On the shadow of rotating traversable wormholes

Quasinormal Modes of Static Ellis-Bronnikov Wormholes

Shadows and Accretion Disk Images of Compact Objects

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