Nonvanishing magnetic flux through the slightly charged Kerr black hole

Kim, Hongsu; Lee, Chul Hoon; Lee, Hyun Kyu

doi:10.1103/physrevd.63.064037

Cited by 12 publications

(7 citation statements)

References 17 publications

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“…Of course, the CM energy is also affected by the radial coordinates of the two particles. We can adjust the parameters in equation (29) to make the CM energy of the two particles diverge at the event horizon of the black hole. Nonetheless, the former type of parameters is the property of the black hole itself and we cannot change it, so we can consider the second type of parameters.…”

Section: Near Horizon Collision In Rotating Bardeen Black Hole Surrou...mentioning

confidence: 99%

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Rotating Bardeen black hole surrounded by perfect fluid dark matter as a particle accelerator

Li,

Zhang,

et al. 2023

Commun. Theor. Phys.

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We study the event horizon of a rotating Bardeen black hole surrounded by perfect fluid dark matter and the black hole as a particle accelerator. The black hole is represented by four parameters: mass $M$, rotation parameter $a$, dark matter parameter $\alpha$ and magnetic charge $g$. It is interesting that when we determine the values of magnetic charge $g$ and dark matter parameters $\alpha$ we can get a critical rotation parameter $a_E$ and then we get a contour plane with $\Delta$= 0 taking three parameters as coordinates. We also derive the effective potential of the particle and the centre-of-mass (CM) energy of the two particles outside the black hole by using the motion equations of the particle in the equatorial plane of the black hole. We find that the CM energy depends not only on the rotation parameter $a$, but also on the parameters $g$ and $\alpha$. We discuss the CM energy for two particles colliding at the black hole horizon in the extreme and non-extreme cases, respectively. It is found that the CM energy can be arbitrarily high when the angular momentum of one of the two particles is the critical angular momentum under the background of extreme black holes and there is no such result for non-extreme black holes, because the particles do not reach the black hole horizon when the angular momentum of the particles is critical angular momentum. Therefore, we prove that the rotating Bardeen black hole surrounded by perfect fluid dark matter can be used as a particle accelerator.

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Section: Near Horizon Collision In Rotating Bardeen Black Hole Surrou...mentioning

confidence: 99%

“…In 1965, Newman and Janis proposed the Newman-Janis algorithm to solve the rotation of regular black hole [27], which has been widely used [25,[28][29][30][31][32][33][34][35]. The metric of the rotating Bardeen black hole surrounded by perfect fluid dark matter [9] was obtained by [36,37] r r q f q q r q f…”

mentioning

confidence: 99%

Rotating Bardeen black hole surrounded by perfect fluid dark matter as a particle accelerator

Li,

Zhang,

et al. 2023

Commun. Theor. Phys.

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“…We would like to stress that the induced charge plays The value of Q max •ind is small in comparison with Qmax implying that its effect on the spacetime geometry can be neglected. The upper boundary for the charge-to-mass ratio for the Galactic centre SMBH (Kim et al 2001) is…”

Section: Charge Induced By Rotating Smbhmentioning

confidence: 99%

On the charge of the Galactic centre black hole

Zajaček

Tursunov

Eckart

et al. 2018

Monthly Notices of the Royal Astronomical Society

131

104

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The Galactic centre supermassive black hole (SMBH), in sharp contrast with its complex environment, is characterized by only three classical parameters -mass, spin, and electric charge. Its charge is poorly constrained. It is, however, usually assumed to be zero because of neutralization due to the presence of plasma. We revisit the question of the SMBH charge and put realistic limits on its value, timescales of charging and discharging, and observable consequences of the potential, small charge associated with the Galactic centre black hole. The electric charge due to classical arguments based on the mass difference between protons and electrons is 10 9 C and is of a transient nature on the viscous time-scale. However, the rotation of a black hole in magnetic field generates electric field due to the twisting of magnetic field lines. This electric field can be associated with induced charge, for which we estimate an upper limit of 10 15 C. Moreover, this charge is most likely positive due to an expected alignment between the magnetic field and the black-hole spin. Even a small charge of this order significantly shifts the position of the innermost stable circular orbit (ISCO) of charged particles. In addition, we propose a novel observational test based on the presence of the bremsstrahlung surface brightness decrease, which is more sensitive for smaller unshielded electric charges than the black-hole shadow size. Based on this test, the current upper observational limit on the charge of Sgr A* is 3 × 10 8 C.

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“…Recently, there has been an increasing interest in charged black holes: see Refs. [22][23][24][25][26][27][28][29][30][31][32][33][34][35][36][37][38][39] and references therein. In Ref.…”

Section: Introductionmentioning

confidence: 99%

Gravitational Waves and Electromagnetic Radiation from Charged Black Hole Binaries

Benavides

Han

2023

Symmetry

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In this manuscript, we investigate the electromagnetic radiation of a binary system of electrically charged black holes. Using the results of previous works, we compute the analytical expression for the waveform, the phase, and the Fourier transform during the inspiral phase for both the electromagnetic and gravitational radiations. To do so, we consider the quasi-circular approximation and small values for the charge-to-mass ratio in each black hole. In the case of electromagnetic radiation, we focus on the dipole contribution, but we also include the quadrupole term to complete our discussion. We found that the gravitational and electromagnetic waveforms contain two terms, and so does the Fourier transform. However, the behavior is dominated only by one of them. In the frequency-domain waves, for example, the dipole and quadrupole contributions and the gravitational wave are dominated by terms proportional to f−3/6, f−1/6 and f−7/6, respectively. As expected, the gravitational radiation and the quadrupole contribution have the same phase, in contrast to the dipole contribution. Moreover, the electromagnetic wave is more sensitive to changes in the charge-to-mass ratio than the gravitational wave.

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Nonvanishing magnetic flux through the slightly charged Kerr black hole

Cited by 12 publications

References 17 publications

Rotating Bardeen black hole surrounded by perfect fluid dark matter as a particle accelerator

Rotating Bardeen black hole surrounded by perfect fluid dark matter as a particle accelerator

On the charge of the Galactic centre black hole

Gravitational Waves and Electromagnetic Radiation from Charged Black Hole Binaries

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