Construction and physical properties of Kerr black holes with scalar hair

Herdeiro, Carlos; Radu, Eugen

doi:10.1088/0264-9381/32/14/144001

Cited by 272 publications

(391 citation statements)

References 152 publications

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“…The explicit form of the coefficients can be found in [15,21]. Note that the parameters b (in [21]) and c t (in [15]) relate as b ¼ −c t . In the following we shall dub these as spheroidal prolate (SP) coordinates, cf.…”

Section: The Black-hole Backgroundsmentioning

confidence: 99%

“…8.33 kpc [36]. The KBHsSH and Kerr solutions that we use are expressed in SP coordinates ðt; r; θ; φÞ, as defined in [15]. In order to relate the SP radial coordinate r expressed in units of M, to a physical distance of 8.33 kpc, we need to fix the mass of Sgr A Ã .…”

Section: Ray-tracing Setup and Shadow Computationsmentioning

confidence: 99%

“…The first (and simplest) such family that was discovered, corresponds to Kerr BHs with scalar hair (KBHsSH) [13] (see also [14,15]). These are solutions of Einstein's gravity minimally coupled to a massive, complex, scalar field.…”

Section: Introductionmentioning

confidence: 99%

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Astrophysical imaging of Kerr black holes with scalar hair

et al. 2016

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We address the astrophysical imaging of a family of deformed Kerr black holes (BHs). These are stationary, asymptotically flat BH spacetimes that are solutions of general relativity minimally coupled to a massive, complex scalar field: Kerr BHs with scalar hair (KBHsSH). Such BHs bifurcate from the vacuum Kerr solution and can be regarded as a horizon within a rotating boson star. In a recent letter [P. V. P. Cunha, C. A. R. Herdeiro, E. Radu, and H. F. Rúnarsson, Phys. Rev. Lett. 115, 211102 (2015).], it was shown that KBHsSH can exhibit very distinct shadows from the ones of their vacuum counterparts. The setup therein, however, considers the light source to be a celestial sphere sufficiently far away from the BH. Here, we analyze KBHsSH surrounded by an emitting torus of matter simulating a more realistic astrophysical environment, and study the corresponding lensing of light as seen by a very faraway observer, to appropriately model ground-based observations of Sgr A Ã . We find that the differences in imaging between KBHsSH and comparable vacuum Kerr BHs remain, albeit less dramatic than those observed for the corresponding shadows in the previous setup. In particular, we highlight two observables that might allow differentiating KBHsSH and Kerr BHs. The first is the angular size of the photon ring (in a Kerr spacetime) or lensing ring (in a KBHSH spacetime), the latter being significantly smaller for sufficiently non-Kerr-like spacetimes. The second is the existence of an edge in the intensity distribution (the photon ring in Kerr spacetime). This edge can disappear for very non-Kerr-like KBHsSH. It is plausible, therefore, that sufficiently precise very long baseline interferometric observations of BH candidates can constrain this model.

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Section: The Black-hole Backgroundsmentioning

confidence: 99%

Section: Ray-tracing Setup and Shadow Computationsmentioning

confidence: 99%

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Astrophysical imaging of Kerr black holes with scalar hair

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“…Consequently, in this setup, the bald Kerr BH is unstable and the scalar field (which is not associated with a Gauss law) grows in time outside the BH. This growth could, in principle, approach an equilibrium configuration, in which the BH becomes hairy, because stationary solutions describing Kerr BHs with (this type of) scalar hair have been recently discovered [13][14][15]. So, is the end point of the superradiant instability triggered by a massive scalar field a hairy Kerr BH?…”

Section: Introductionmentioning

confidence: 99%

“…We found that, indeed, the generic final state is a hairy BH: a charged horizon, surrounded by a scalar field condensate storing part of the charge and energy of the initial BH. This condensate's phase oscillates at the threshold frequency of the superradiant instability, thus realizing dynamically charged hairy BHs analogous to Kerr BHs with scalar hair [13][14][15]. The former have recently been constructed as stationary solutions, and a subset was shown to be perturbatively stable [27].…”

Section: Introductionmentioning

confidence: 99%

Dynamical formation of a Reissner-Nordström black hole with scalar hair in a cavity

et al. 2016

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In a recent Letter [Sanchis-Gual et al., Phys. Rev. Lett. 116, 141101 (2016)], we presented numerical relativity simulations, solving the full Einstein-Maxwell-Klein-Gordon equations, of superradiantly unstable Reissner-Nordström black holes (BHs), enclosed in a cavity. Low frequency, spherical perturbations of a charged scalar field trigger this instability. The system's evolution was followed into the nonlinear regime, until it relaxed into an equilibrium configuration, found to be a hairy BH: a charged horizon in equilibrium with a scalar field condensate, whose phase is oscillating at the (final) critical frequency. Here, we investigate the impact of adding self-interactions to the scalar field. In particular, we find sufficiently large self-interactions suppress the exponential growth phase, known from linear theory, and promote a nonmonotonic behavior of the scalar field energy. Furthermore, we discuss in detail the influence of the various parameters in this model: the initial BH charge, the initial scalar perturbation, the scalar field charge, the mass, and the position of the cavity's boundary (mirror). We also investigate the "explosive" nonlinear regime previously reported to be akin to a bosenova. A mode analysis shows that the "explosions" can be interpreted as the decay into the BH of modes that exit the superradiant regime.

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Superradiance

Brito¹,

Cardoso²,

Pani³

2020

Lecture Notes in Physics

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The series Lecture Notes in Physics (LNP), founded in 1969, reports new developments in physics research and teaching -quickly and informally, but with a high quality and the explicit aim to summarize and communicate current knowledge in an accessible way. Books published in this series are conceived as bridging material between advanced graduate textbooks and the forefront of research and to serve three purposes:• to be a compact and modern up-to-date source of reference on a well-defined topic. • to serve as an accessible introduction to the field to postgraduate students and nonspecialist researchers from related areas. • to be a source of advanced teaching material for specialized seminars, courses and schools.Both monographs and multi-author volumes will be considered for publication. Edited volumes should, however, consist of a very limited number of contributions only. Proceedings will not be considered for LNP.Volumes published in LNP are disseminated both in print and in electronic formats, the electronic archive being available at springerlink.com. The series content is indexed, abstracted and referenced by many abstracting and information services, bibliographic networks, subscription agencies, library networks, and consortia.

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Construction and physical properties of Kerr black holes with scalar hair

Cited by 272 publications

References 152 publications

Astrophysical imaging of Kerr black holes with scalar hair

Astrophysical imaging of Kerr black holes with scalar hair

Dynamical formation of a Reissner-Nordström black hole with scalar hair in a cavity

Superradiance

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