Shadow of a charged black hole with scalar hair

Guo, Wen-Di; Wei, Shao-Wen; Liu, Yu-Xiao

doi:10.1140/epjc/s10052-023-11316-1

Cited by 18 publications

(5 citation statements)

References 94 publications

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“…Therefore, we reach the important conclusion that the structure of the Grassmann tensor network and the contraction rule are not affected by the gauge fields. The resulting coefficient tensor in equation ( 60) has the same expression as equation (40), which was the coefficient tensor for the pure fermionic model in equation (1). The exact contractions among the Grassmann tensors result in those among the coefficient tensors, with or without the lattice gauge fields.…”

Section: Extension To Lattice Gauge Theoriesmentioning

confidence: 98%

“…where the coefficient tensor of M has been already derived in equation (40) or equation (60). The HOTRG for the Grassmann tensor network should provide us with the coarsegraining transformation such as…”

Section: Approximate Contraction By the Levin-nave Trgmentioning

confidence: 99%

“…This new approach is called the tensor RG (TRG). The TRG approach allows us to interpret and quantitatively realize the traditional RG ideas in the language of the tensor network [20,[35][36][37][38][39][40][41].…”

Section: Introductionmentioning

confidence: 99%

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Tensor renormalization group for fermions

Akiyama,

Meurice,

Sakai

2024

J. Phys.: Condens. Matter

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We review the basic ideas of the Tensor Renormalization Group method and show how they can be applied for lattice field theory models involving relativistic fermions and Grassmann variables in arbitrary dimensions. We discuss recent progress for entanglement filtering, loop optimization, bond-weighting techniques and matrix product decompositions for Grassmann tensor networks. The new methods are tested with two-dimensional Wilson--Majorana fermions and multi-flavor Gross--Neveu models. We show that the methods can also be applied to the fermionic Hubbard model in 1+1 and 2+1 dimensions.

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Section: Extension To Lattice Gauge Theoriesmentioning

confidence: 98%

Section: Approximate Contraction By the Levin-nave Trgmentioning

confidence: 99%

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Tensor renormalization group for fermions

Akiyama,

Meurice,

Sakai

2024

J. Phys.: Condens. Matter

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“…In the Hamiltonian formalism, the geodetic motion of a particle of, possibly zero, mass µ moving in a metric g µν is governed by the Hamiltonian [22,65,66]…”

Section: Light Ringsmentioning

confidence: 99%

On the stability and deformability of top stars

Bianchi,

Di Russo,

Grillo

et al. 2023

J. High Energ. Phys.

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Topological stars, or top stars for brevity, are smooth horizonless static solutions of Einstein-Maxwell theory in 5-d that reduce to spherically symmetric solutions of Einstein-Maxwell-Dilaton theory in 4-d. We study linear scalar perturbations of top stars and argue for their stability and deformability. We tackle the problem with different techniques including WKB approximation, numerical analysis, Breit-Wigner resonance method and quantum Seiberg-Witten curves. We identify three classes of quasi-normal modes corresponding to prompt-ring down modes, long-lived meta-stable modes and what we dub ‘highly-damped’ modes. All mode frequencies we find have negative imaginary parts, thus suggesting linear stability of top stars. Moreover we determine the tidal Love and dissipation numbers encoding the response to tidal deformations and, similarly to black holes, we find zero value in the static limit but, contrary to black holes, we find non-trivial dynamical Love numbers and vanishing dissipative effects at linear order. For the sake of illustration in a simpler context, we also consider a toy model with a piece-wise constant potential and a centrifugal barrier that captures most of the above features in a qualitative fashion.

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“…Furthermore, the QNM frequencies can also partly reveal the stability of the background space-time under small perturbations [48,49]. QNMs play very important roles in other physical systems, for example, leaky resonant cavities [50], and brane world models [51][52][53], which have been widely studied [54][55][56][57][58][59][60][61][62].…”

Section: Introductionmentioning

confidence: 99%

Quasinormal Modes of a Charged Black Hole with Scalar Hair

Guo

Tan

2023

Universe

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Based on the five-dimensional Einstein–Maxwell theory, Bah et al. constructed a singularity-free topology star/black hole [Phys. Rev. Lett. 126, 151101 (2021)]. After performing the Kaluza–Klein reduction, i.e., integrating the extra space dimension, it can obtain an effective four-dimensional spherically static charged black hole with scalar hair. In this paper, we study the quasinormal modes (QNMs) of the scalar, electromagnetic, and gravitational fields in the background of this effective four-dimensional charged black hole. The radial parts of the perturbed fields all satisfy a Schrödinger-like equation. Using the asymptotic iteration method, we obtain the QNM frequencies semianalytically. For low-overtone QNMs, the results obtained using both the asymptotic iteration method and the Wentzel–Kramers–Brillouin approximation method agree well. In the null coordinates, the evolution of a Gaussian package is also studied. The QNM frequencies obtained by fitting the evolution data also agree well with the results obtained using the asymptotic iteration method.

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Shadow of a charged black hole with scalar hair

Cited by 18 publications

References 94 publications

Tensor renormalization group for fermions

Tensor renormalization group for fermions

On the stability and deformability of top stars

Quasinormal Modes of a Charged Black Hole with Scalar Hair

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