Infinitesimally thin static scalar shells surrounding charged Gauss-Bonnet black holes

Hod, Shahar

doi:10.1007/jhep02(2022)039

Cited by 6 publications

(6 citation statements)

References 38 publications

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“…We note that, similar to the four-dimensional case shown in Ref. [33], in the subcritical charge regime with a positive coupling parameter η, thin static massive scalar field can also be supported by the higher-dimensional RN black hole. However, in that case, the scalar configuration is connected to the event horizon of the black hole as r p < r + .…”

Section: Closing Remarkssupporting

confidence: 78%

“…[33], here in the higher dimensional cases, it is worth noting a point that the super-critical charge regime parameter Cd which makes the radial peak of the GB invariant (25) coincide with the event horizon has a nontrivial change from d = 4 to d ≥ 5. That is, we have C4 = 0.91652 [33]; it increases to C5 = 0.93696 but then decreases with the increasing spacetime dimension d (this is not relevant to whether d is even or odd, as we have C8 = 0.90198, cf. ( 27)).…”

Section: Closing Remarksmentioning

confidence: 97%

“…Following the suggestion of Ref. [33], we here define two auxiliary dimensionless variables χ and x by relations [cf. Eqs.…”

Section: Quasinormal Resonance Spectrum Of the Black Hole-massive Sca...mentioning

confidence: 99%

“…However, in Ref. [33], infinitesimally thin static scalar shell surrounding the four-dimensional RN black hole in the framework of EMsGB was studied and an analytical resonance spectrum formula as a sharp boundary between bald and hairy RN black hole-massive scalar field configurations was obtained in large mass (or large coupling) regime.…”

Section: Introductionmentioning

confidence: 99%

“…In the present paper, we will mainly follow Ref. [33] and extend the study to higher-dimensional case. We will analytically derive the resonance spectrum of the coupling parameter as critical existence-line characterizing cloudy higher dimensional RN black hole.…”

Section: Introductionmentioning

confidence: 99%

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Higher dimensional Reissner-Nordström black holes supporting static scalar shells

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Section: Closing Remarkssupporting

confidence: 78%

Section: Closing Remarksmentioning

confidence: 97%

“…Following the suggestion of Ref. [33], we here define two auxiliary dimensionless variables χ and x by relations [cf. Eqs.…”

Section: Quasinormal Resonance Spectrum Of the Black Hole-massive Sca...mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Higher dimensional Reissner-Nordström black holes supporting static scalar shells

et al. 2022

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Spin-charge induced scalarization of Kerr-Newman black-hole spacetimes

Hod

2022

J. High Energ. Phys.

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It has recently been demonstrated that Reissner-Nordström black holes in composed Einstein-Maxwell-scalar field theories can support static scalar field configurations with a non-minimal negative coupling to the Maxwell electromagnetic invariant of the charged spacetime. We here reveal the physically interesting fact that scalar field configurations with a non-minimal positive coupling to the spatially-dependent Maxwell electromagnetic invariant $$ \mathcal{F} $$ F ≡ FμνFμν can also be supported in black-hole spacetimes. Intriguingly, it is explicitly proved that the positive-coupling black-hole spontaneous scalarization phenomenon is induced by a non-zero combination a ∙ Q ≠ 0 of both the spin a ≡ J/M and the electric charge Q of the central supporting black hole. Using analytical techniques we prove that the regime of existence of the positive-coupling spontaneous scalarization phenomenon of Kerr-Newman black holes with horizon radius r+(M, a, Q) and a non-zero electric charge Q (which, in principle, may be arbitrarily small) is determined by the critical onset line (a/r+)critical = $$ \sqrt{2} $$ 2 − 1. In particular, spinning and charged Kerr-Newman black holes in the composed Einstein-Maxwell-scalar field theory are spontaneously scalarized by the positively coupled fields in the dimensionless charge regime $$ 0<\frac{Q}{M}\le \sqrt{2\sqrt{2}-2} $$ 0 < Q M ≤ 2 2 − 2 if their dimensionless spin parameters lie above the critical onset line $$ \frac{a(Q)}{M}\ge {\left[\frac{a(Q)}{M}\right]}_{\mathrm{critical}}=\frac{1+\sqrt{1-2\left(2-\sqrt{2}\right){\left(Q/M\right)}^2}}{2\sqrt{2}} $$ a Q M ≥ a Q M critical = 1 + 1 − 2 2 − 2 Q / M 2 2 2 .

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Analytic study of the Maxwell electromagnetic invariant in spinning and charged Kerr-Newman black-hole spacetimes

Hod

2023

J. High Energ. Phys.

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The Maxwell invariant plays a fundamental role in the mathematical description of electromagnetic fields in charged spacetimes. In particular, it has recently been proved that spatially regular scalar fields which are non-minimally coupled to the Maxwell electromagnetic invariant can be supported by spinning and charged Kerr-Newman black holes. Motivated by this physically intriguing property of asymptotically flat black holes in composed Einstein-Maxwell-scalar field theories, we present a detailed analytical study of the physical and mathematical properties of the Maxwell electromagnetic invariant $$ {\mathcal{F}}_{\textrm{KN}}\left(r,\theta; M,a,Q\right) $$ F KN r θ M a Q which characterizes the Kerr-Newman black-hole spacetime [here {r, θ} are respectively the radial and polar coordinates of the curved spacetime and {M, J = M a, Q} are respectively the mass, angular momentum, and electric charge parameters of the black hole]. It is proved that, for all Kerr-Newman black-hole spacetimes, the spin and charge dependent minimum value of the Maxwell electromagnetic invariant is attained on the equator of the black-hole surface. Interestingly, we reveal the physically important fact that Kerr-Newman spacetimes are characterized by two critical values of the dimensionless rotation parameter $$ \hat{a}\equiv a/{r}_{+} $$ a ̂ ≡ a / r + [here r+ (M, a, Q) is the black-hole horizon radius], $$ {\hat{a}}_{\textrm{crit}}^{-}=\sqrt{3-2\sqrt{2}} $$ a ̂ crit − = 3 − 2 2 and $$ {\hat{a}}_{\textrm{crit}}^{+}=\sqrt{5-2\sqrt{5}} $$ a ̂ crit + = 5 − 2 5 , which mark the boundaries between three qualitatively different spatial functional behaviors of the Maxwell electromagnetic invariant: (i) Kerr-Newman black holes in the slow-rotation $$ \hat{a}<{\hat{a}}_{\textrm{crit}}^{-} $$ a ̂ < a ̂ crit − regime are characterized by negative definite Maxwell electromagnetic invariants that increase monotonically towards spatial infinity, (ii) for black holes in the intermediate spin regime $$ {\hat{a}}_{\textrm{crit}}^{-}\le \hat{a}\le {\hat{a}}_{\textrm{crit}}^{+} $$ a ̂ crit − ≤ a ̂ ≤ a ̂ crit + , the positive global maximum of the Kerr-Newman Maxwell electromagnetic invariant is located at the black-hole poles, and (iii) Kerr-Newman black holes in the super-critical regime $$ \hat{a}<{\hat{a}}_{\textrm{crit}}^{+} $$ a ̂ < a ̂ crit + are characterized by a non-monotonic spatial behavior of the Maxwell electromagnetic invariant $$ {\mathcal{F}}_{\textrm{KN}}\left(r={r}_{+},\theta; M,a,Q\right) $$ F KN r = r + θ M a Q along the black-hole horizon with a spin and charge dependent global maximum whose polar angular location is characterized by the dimensionless functional relation $$ {\hat{a}}^2 $$ a ̂ 2 · (cos2θ)max = 5 – $$ 2\sqrt{5} $$ 2 5 .

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Infinitesimally thin static scalar shells surrounding charged Gauss-Bonnet black holes

Cited by 6 publications

References 38 publications

Higher dimensional Reissner-Nordström black holes supporting static scalar shells

Higher dimensional Reissner-Nordström black holes supporting static scalar shells

Spin-charge induced scalarization of Kerr-Newman black-hole spacetimes

Analytic study of the Maxwell electromagnetic invariant in spinning and charged Kerr-Newman black-hole spacetimes

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