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Scalarized black holes in the Einstein-Maxwell-scalar theory with a quasitopological term

Yun Soo Myung and De-Cheng Zou
Phys. Rev. D 103, 024010 – Published 6 January 2021
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  • INTRODUCTION
  • SCALAR COUPLING TO MAXWELL TERM
  • SCALAR COUPLING TO A QUASITOPOLOGICAL…
  • SCALAR COUPLING TO MAXWELL AND…
  • DISCUSSIONS
  • ACKNOWLEDGMENTS
    • References

    Abstract

    We investigate the Einstein-Maxwell-scalar theory with a quasitopological term. Considering exponential couplings to a Maxwell term, to a quasitopological term, and to both terms, we obtain three sets of infinite scalarized charged black holes by taking into account tachyonic instability of a dyonic Reissner-Nordström black hole. Each set of infinite scalarized charged black holes is classified by the number of n=0,1,2,…, where n=0 is called the fundamental black hole and n=1,2,… denote the n-excited black holes. All n=0 black holes are stable against the radial perturbation, while all n=1, 2 black holes are unstable.

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    • Received 20 November 2020
    • Accepted 22 December 2020

    DOI:https://doi.org/10.1103/PhysRevD.103.024010

    © 2021 American Physical Society

    Physics Subject Headings (PhySH)

    1. Research Areas
    Alternative gravity theories
    Gravitation, Cosmology & Astrophysics

    Authors & Affiliations

    Yun Soo Myung1,* and De-Cheng Zou1,2,†

    • 1Institute of Basic Sciences and Department of Computer Simulation, Inje University, Gimhae 50834, Korea
    • 2Center for Gravitation and Cosmology and College of Physical Science and Technology, Yangzhou University, Yangzhou 225009, China

    • *ysmyung@inje.ac.kr
    • †dczou@yzu.edu.cn

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    Issue

    Vol. 103, Iss. 2 — 15 January 2021

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    Images

    • Figure 1
      Figure 1

      The α-dependent potentials as function of r∈[r+,10] with the outer horizon radius r+=1.652(Q=0.7,P=0.3) and l=0. Curves represent the potential VdRN(r,0.7,0.3,1,α) with different α=5,8,αth=9.451, 15.

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    • Figure 2
      Figure 2

      Left: plot of an unstable scalar mode with Q=0.7 and P=0.3. The y(x) axis denotes Ω in eΩt (α). We observe that the threshold of instability (•:Ω=0) is located at αth=9.451. Right: radial profiles of φ(r)=u(r)/r as function of r∈[r+=1.651,30] for the first three scalar clouds with Q=0.7 and P=0.3. These solutions φn(r) are classified by the order number n=0, 1, 2 which is identified by the number of nodes (zero crossings).

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    • Figure 3
      Figure 3

      Plots of a scalarized charged black hole with α=54 belonging to the n=0 branch of α≥α0=9.451. Here, the horizon is located at r=r+=1.651 (lnr+=0.503) and two parameters are given by ϕ0=0.1231 and δ0=0.0054. f(r) and v¯(r) represent those for the dyonic RN black with ϕ¯(r)=δ¯(r)=0.

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    • Figure 4
      Figure 4

      Scalar potentials Vmt(r,α) around n=0 [(a) α≥9.451], 1 [(b) α≥47.414], 2 [(c) α≥115.72] black holes in the infinite branches. The positive barriers in the near horizon become smaller and smaller as n increases.

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    • Figure 5
      Figure 5

      Left: plots of ωi=Ω(ωr=0) as functions of α for (l=0)-scalar mode around the n=0(α≥9.451), 1(α≥47.414), 2(α≥115.72) black holes with Q=0.7 and P=0.3. Right: plots of the reduced entropy aH as a function of α with fixed Q=0.7 and P=0.3.

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    • Figure 6
      Figure 6

      Radial profiles of φn(r) as function of r∈[r+=0.9078,6] for the first three perturbed scalar solutions with Q=0.7 and P=0.8.

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    • Figure 7
      Figure 7

      Scalar potentials Vqtt(r,α) around n=0 [(a) α≥4.933], 1 [(b) α≥18.687], 2 [(c) α≥45.590] black holes. The positive barriers in the near horizon become smaller and smaller as n increases.

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    • Figure 8
      Figure 8

      Left: plots of ωi=Ω as functions of α for (l=0)-scalar mode around the n=0(α≥4.933), 1(α≥18.687), 2(α≥45.590) black holes with Q=0.7 and P=0.8. Right: plots of the reduced entropy aH as a function of α with fixed Q=0.7 and P=0.8.

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    • Figure 9
      Figure 9

      Radial profiles of φn(r) as function of r∈[r+=?,6] for the first three perturbed scalar solutions with Q=0.7 and P=0.3.

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    • Figure 10
      Figure 10

      Scalar potentials Vmqt(r,α) around n=0 [(a) α≥9.187], 1 [(b) α≥46.236], 2 [(c) α≥112.901] black holes. The positive barriers in the near horizon become smaller and smaller as n increases.

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    • Figure 11
      Figure 11

      Left: plots of ωi=Ω as functions of α for (l=0)-scalar mode around the n=0(α≥9.1987), 1(α≥46.236), 2(α≥112.901) black holes with Q=0.7 and P=0.3. Right: plots of the reduced entropy aH as a function of α with fixed Q=0.7 and P=0.3.

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