Rotating Wormholes

Kleihaus, Burkhard; Kunz, Jutta

doi:10.1007/978-3-319-55182-1_3

Cited by 6 publications

(9 citation statements)

References 36 publications

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“…Due to the non-trivial topology, however, also wormhole solutions appear, where the matter is distributed unevenly with respect to the spacetime regions on either side of the throat. These asymmetric wormholes always appear in pairs, where the two solutions of a pair are again related via reflection symmetry.Ellis wormholes may also rotate [23][24][25][26][27]. A rotation of the throat can be induced by an appropriate choice of the boundary conditions, allowing for asymptotic flatness in the two asymptotic regions, which, however, are rotating with respect to one another.…”

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confidence: 99%

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Symmetric and asymmetric wormholes immersed in rotating matter

et al. 2018

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We consider four-dimensional wormholes immersed in bosonic matter. While their existence is based on the presence of a phantom field, many of their interesting physical properties are bestowed upon them by an ordinary complex scalar field, which carries only a mass term, but no self-interactions. For instance, the rotation of the scalar field induces a rotation of the throat as well. Moreover, the bosonic matter need not be symmetrically distributed in both asymptotically flat regions, leading to symmetric and asymmetric rotating wormhole spacetimes. The presence of the rotating matter also allows for wormholes with a double throat.In General Relativity the non-trivial topology of wormholes can be achieved by allowing for the presence of exotic matter [1][2][3][4][5][6][7][8]. In the simplest case, a massless phantom (scalar) field can be chosen, whose Lagrangian carries the opposite sign as compared to the one of an ordinary scalar field. The resulting Ellis wormholes are static spherically symmetric solutions, connecting two asymptotically flat regions of space-time.Ellis wormholes may also be coupled to matter fields. For instance, they may be filled by nuclear matter [9-14], they may be threaded by chiral (Skyrmionic) matter [15], or they may be immersed in bosonic matter consisting of an ordinary complex boson field with self-interaction [16,17], or with only a mass term present [18].As in the case of non-topological solitons and boson stars [19][20][21][22] the boson field then has a harmonic timedependence, allowing for localized matter fields surrounding a static throat. Since the time-dependence cancels in the stress-energy tensor, the resulting metric is static. Clearly, there are symmetric wormholes, where the matter is distributed symmetrically on either side of the throat. Thus these symmetric wormholes possess reflection symmetry. Due to the non-trivial topology, however, also wormhole solutions appear, where the matter is distributed unevenly with respect to the spacetime regions on either side of the throat. These asymmetric wormholes always appear in pairs, where the two solutions of a pair are again related via reflection symmetry.Ellis wormholes may also rotate [23][24][25][26][27]. A rotation of the throat can be induced by an appropriate choice of the boundary conditions, allowing for asymptotic flatness in the two asymptotic regions, which, however, are rotating with respect to one another. On the other hand, a rotation of the throat can also be induced by immersing the throat into rotating matter [18]. In that case, the boundary conditions can be chosen symmetrically in the two asymptotic regions, and thus these need not rotate with respect to one another.These wormholes immersed in rotating matter possess interesting properties [18]. Depending on their physical parameters, their geometry can change from exhibiting a single throat to developing an equator surrounded by a throat on either side, i.e., these wormholes then feature a double throat geometry. These wormholes also possess ergoregi...

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“…Ellis wormholes may also rotate [23][24][25][26][27]. A rotation of the throat can be induced by an appropriate choice of the boundary conditions, allowing for asymptotic flatness in the two asymptotic regions, which, however, are rotating with respect to one another.…”

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Symmetric and asymmetric wormholes immersed in rotating matter

et al. 2018

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“…As mentioned in the Introduction, the stability of these wormhole geometries is of great importance, but lies outside the scope of this work. However, a future line of research lies in applying a similar analysis as considered in [30,31] to these solutions using three-forms. Another application is to construct evolving wormhole geometries, such as finding solutions in a cosmological background, which are conformally related to the respective static geometries, as outlined in [50][51][52][53].…”

Section: Discussionmentioning

confidence: 99%

“…However, in wormhole geometries, the non-trivial topology is supported by a phantom scalar field, in order to satisfy the flaring-out condition. In particular, rotating wormhole solutions in GR were presented, which are supported by a phantom scalar field [30,31]. These specific solutions evolved from a static Ellis wormhole configuration, when the throat is set into rotation, and as the rotational velocity increases, the throat deforms until an extremal Kerr solution is obtained, at a maximal value of the rotational velocity.…”

Section: Introductionmentioning

confidence: 99%

Wormhole geometries supported by three-form fields

Barros

Lobo

2018

Phys. Rev. D

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In this work, we find novel static and spherically symmetric wormhole geometries using a threeform field. By solving the gravitational field equations, we find a variety of analytical and numerical solutions and show that it is possible for the matter fields threading the wormhole to satisfy the null and weak energy conditions throughout the spacetime, when the three-form field is present. In these cases, the form field is responsible for supporting the wormhole and all the exoticity is confined to it. Thus, the three-form curvature terms, which may be interpreted as a gravitational fluid, sustain these wormhole geometries. We also show that in the case of a vanishing redshift function the field can display a cosmological constant behavior.

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“…The static solutions were obtained in analytical form by Ellis [60] and Bronnikov [61] and their properties were investigated in a number of works [62][63][64][65]. Their rotating generalizations have been constructed perturbatively [66,67] and numerically [68][69][70]. Here we consider quasi-periodic oscillations in accretion disks around symmetric rotating Ellis wormholes [68,69].…”

Section: Introductionmentioning

confidence: 99%

Quasi-periodic Oscillations in Rotating Ellis Wormhole Spacetimes

Deligianni,

Kleihaus,

Kunz

et al. 2021

Preprint

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We analyze the properties of the circular orbits for massive particles in the equatorial plane of symmetric rotating Ellis wormholes. In particular, we obtain the orbital frequencies and the radial and vertical epicyclic frequencies, and consider their lowest parametric, forced and Keplerian resonances. These show that quasi-periodic oscillations in accretion disks around symmetric rotating Ellis wormholes have many distinct properties as compared to quasi-periodic oscillations in accretion disks around rotating Teo wormholes and the Kerr black hole. Still we can distinguish some common features which appear in wormhole spacetimes as opposed to black holes. The most significant ones include the possibility of excitation of stronger resonances such as lower order parametric and forced resonances and the localization of these resonances deep in the region of strong gravitational interaction near the wormhole throat, which will lead to further amplification of the signal.

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Rotating Wormholes

Cited by 6 publications

References 36 publications

Symmetric and asymmetric wormholes immersed in rotating matter

Symmetric and asymmetric wormholes immersed in rotating matter

Wormhole geometries supported by three-form fields

Quasi-periodic Oscillations in Rotating Ellis Wormhole Spacetimes

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