Gravitating vortons as ring solitons in general relativity

Kunz, Jutta; Radu, Eugen; Subagyo, Bintoro Anang

doi:10.1103/physrevd.87.104022

Cited by 8 publications

(23 citation statements)

References 83 publications

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“…They are made from loops of vortices, which are balanced against collapse by rotation, and share many features of the Q-balls. In particular, as shown in [33], gravitating vortons may posses an ergoregion with a toroidal shape. Thus their BH generalization will also possess ergo-Saturns [21].…”

Section: Further Remarksmentioning

confidence: 99%

Ergosurfaces for Kerr black holes with scalar hair

2014

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We have recently reported the existence of Kerr black holes with scalar hair in General Relativity minimally coupled to a massive, complex scalar field [C. Herdeiro and E. Radu, Phys. Rev. Lett. 112, 221101 (2014)]. These solutions interpolate between boson stars and Kerr black holes. The latter have a well-known topologically S 2 ergosurface (ergosphere) whereas the former develop a S 1 × S 1 ergosurface (ergotorus) in a region of parameter space. We show that hairy black holes always have an ergoregion, and that this region is delimited by either an ergosphere or an ergo-Saturn-i.e. a S 2 ⊕ðS 1 × S 1 Þ ergosurface. In the phase space of solutions, the ergotorus can either appear disconnected from the ergosphere or pinch off from it. We provide a heuristic argument, based on a measure of the size of the ergoregion, that superradiant instabilities-which are likely to be present-are weaker for hairy black holes than for Kerr black holes with the same global charges. We observe that Saturn-like, and even more remarkable, ergosurfaces should also arise for other rotating "hairy" black holes.

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Section: Further Remarksmentioning

confidence: 99%

Ergosurfaces for Kerr black holes with scalar hair

2014

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“…They represent a new family of mini boson stars, which do not possess a flat space limit. The dependence of these solutions on the frequency ω is qualitatively similar to that of the spinning boson stars, that can be linked to flat space Q-balls because of the presence of higher order self-interaction terms, and other gravitating solitons [11,19,[27][28][29][30][31]. The existence region of the spinning axially symmetric solutions is limited by ω max = µ from above and some ω min > 0 from below.…”

Section: Numerical Resultsmentioning

confidence: 75%

“…The structure of the dynamical equation (9) suggests that, analogous to the case of the spinning axially-symmetric Q-balls and boson stars [27][28][29][30][31][32], the hairy BH solutions of the Einstein-Klein-Gordon system may also be either symmetric with respect to reflections in the equatorial plane, θ → π − θ, or antisymmetric, as conjectured in [9]. The solutions of the first type are referred to as parity-even, while the configurations of the second type are termed parity-odd.…”

Section: A Spinning Axially-symmetric Configurationsmentioning

confidence: 99%

Kerr black holes with parity-odd scalar hair

2019

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We study Kerr black holes with synchronised non-trivial parity-odd massive scalar hair in four dimensional asymptotically flat space-time. These axially symmetric stationary spinning solutions of the minimally coupled Einstein-Klein-Gordon theory provide yet another example of bound states in synchronous rotation with the event horizon. We discuss the properties of these parity-odd hairy black holes and boson stars and exhibit their domain of existence. Considering the ergo-regions of these hairy black holes, we show that apart from the previously discussed ergo-sphere and ergo-Saturn, they support a new type of composite ergo-surfaces with the topology of a double-torus-Saturn (S 1 × S 1 ) (S 1 × S 1 ) S 2 .

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“…While Garfinkle and coauthors have considered fully self-consistent models in the case of straight strings, we are unaware of similar studies in the circular case. Kunz et al [28] have numerically modeled gravitating toroidal configurations of U (1) × U (1) gauge-fields (so-called vortons), but they do not discuss a deficit angle.…”

Section: Discussionmentioning

confidence: 99%

Cosmic string and black hole limits of toroidal Vlasov bodies in general relativity

2019

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We numerically investigate limits of a two-parameter family of stationary solutions to the Einstein-Vlasov system. The solutions are toroidal and have non-vanishing angular momentum. As one tunes to more relativistic solutions (measured for example by an increasing redshift) there exists a sequence of solutions which approaches the extreme Kerr black hole family. Solutions with angular momentum larger than the square of the mass are also investigated, and in the relativistic limit the near-field geometry of such solutions is observed to become conical in the sense that there is a deficit angle. Such solutions may provide self-consistent models for rotating circular cosmic strings.

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Gravitating vortons as ring solitons in general relativity

Cited by 8 publications

References 83 publications

Ergosurfaces for Kerr black holes with scalar hair

Ergosurfaces for Kerr black holes with scalar hair

Kerr black holes with parity-odd scalar hair

Cosmic string and black hole limits of toroidal Vlasov bodies in general relativity

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