Chaotic motion around a black hole under minimal length effects

Guo, Xiansheng; Liang, Kangkai; Mu, Benrong; Wang, Peng; Yang, Mingtao

doi:10.1140/epjc/s10052-020-8335-6

Cited by 12 publications

(5 citation statements)

References 58 publications

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“…These chaotic structures can be used to explain intense continuous emissions from black hole-disk systems and provide a wide frequency range in the emitted radiation (Misra et al 2004;Guo et al 2020). The amplitude of the radiation changes over time, and these systems may also be sources of sudden bursts (Cao et al 2023).…”

Section: Exploring the Differences: Disk Dynamics Under Kerr And Egb ...mentioning

confidence: 99%

Perturbing the Stable Accretion Disk in Kerr and 4D Einstein–Gauss–Bonnet Gravities: Comprehensive Analysis of Instabilities and Dynamics

Donmez

2024

Res. Astron. Astrophys.

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The study of a disturbed accretion disk holds great significance in the realm of astrophysics, as such events play a crucial role in revealing the nature of disk structure, the release of energy, and the generation of shock waves. Consequently, they can help explain the causes of X-ray emissions observed in black hole accretion disk systems. In this paper, we perturb the stable disk formed by spherical accretion around Kerr and EGB black holes. This perturbation reveals one- and two-armed spiral shock waves around the black hole. We find a strong connection between these waves and the black hole spin parameter (a/M) and the EGB coupling constant (\alpha). Specifically, we found that as \alpha increases in the negative direction, the dynamics of the disk and the waves become more chaotic. Additionally, we observe that the angular momentum of the perturbing matter significantly affects mass accretion and the oscillation of the arising shock waves. This allows us to observe changes in QPO frequencies. Particularly, perturbations with angular momentum matching the observed C- type low-frequency QPOs of the GRS 1915 + 105 source. Thus, we conclude that the possibility of the occurrence of shock waves within the vicinity of GRS 1915 + 105 is substantial.

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Section: Exploring the Differences: Disk Dynamics Under Kerr And Egb ...mentioning

confidence: 99%

Perturbing the Stable Accretion Disk in Kerr and 4D Einstein–Gauss–Bonnet Gravities: Comprehensive Analysis of Instabilities and Dynamics

Donmez

2024

Res. Astron. Astrophys.

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“…Therefore, for a/M = 0.9, unexpected behavior has been observed for these α values. These chaotic structures can be used to explain intense continuous emissions from the black hole-disk systems and provides a wide frequency range in the emitted radiation (Misra et al 2004;Guo et al 2020). The amplitude of the radiation changes over time.…”

Section: Exploring the Differences: Disk Dynamics Under Kerr And Egb ...mentioning

confidence: 99%

Study of Asymptotic Velocity in the Bondi–Hoyle Accretion Flows in the Domain of Kerr and 4-D Einstein–Gauss–Bonnet Gravities

2022

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Understanding the physical structures of the accreted matter very close to a black hole in quasars and active galactic nucleus (AGN) is an important milestone to constrain the activities occurring in their centers. In this paper, we numerically investigate the effects of the asymptotic velocities on the physical structures of the accretion disk around the Kerr and Einstein–Gauss–Bonnet (EGB) rapidly rotating black holes. The Bondi–Hoyle accretion is considered with a falling gas towards the black hole in an upstream region of the computational domain. Shock cones are naturally formed in the downstream part of the flow around both black holes. The structure of the cones and the amount of the accreted matter depend on asymptotic velocity V∞ (Mach number) and the types of the gravities (Kerr or EGB). Increasing the Mach number of the in-flowing matter in the supersonic region reduces the shock opening angle and the accretion rates, because of the gas rapidly falling towards the black hole. The EGB gravity leads to an increase in the shock opening angle of the shock cones while the mass-accretion rates dM/dt decrease in EGB gravity with a Gauss–Bonnet (GB) coupling constant α. It is also confirmed that accretion rates and drag forces are significantly altered in the EGB gravity. Our numerical simulation results could be used in identifying the accretion mechanism and physical properties of the accretion disk and black hole in the observed X-rays such as NGC 1313 X-1 and 1313 X-2 and MAXI J1803-298.

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“…Such a deformation also affects the Heisenberg uncertainty principle (HUP), and as a result, the generalized uncertainty principle (GUP) has to be used instead of the HUP. Recently, with increasing interest, we observe that many papers examine the effect of the GUP formalism on black hole physics and thermodynamics [26][27][28][29][30][31][32][33][34][35][36][37][38][39][40][41][42][43][44][45]. One of the common features of these studies is the modification of the Hawking radiation.…”

Section: Introductionmentioning

confidence: 99%

Quantum corrections to the thermodynamics of rotating charged BTZ black hole in gravity's rainbow

Lütfüoğlu,

Hamil,

Dahbi

2022

Preprint

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In this manuscript we investigate the thermal properties of the rotating charged BTZ black hole under the GR formalism at first according to the usual Heisenberg algebra. Then, we consider a deformed algebra which leads to a change in the Heisenberg uncertainty principle, and compare the Hawking temperature, entropy, thermodynamical volume, pressure and heat capacity functions with the previous results. Thus, we understand and interpret the quantum effects on the BTZ black hole.

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Chaotic motion around a black hole under minimal length effects

Cited by 12 publications

References 58 publications

Perturbing the Stable Accretion Disk in Kerr and 4D Einstein–Gauss–Bonnet Gravities: Comprehensive Analysis of Instabilities and Dynamics

Perturbing the Stable Accretion Disk in Kerr and 4D Einstein–Gauss–Bonnet Gravities: Comprehensive Analysis of Instabilities and Dynamics

Study of Asymptotic Velocity in the Bondi–Hoyle Accretion Flows in the Domain of Kerr and 4-D Einstein–Gauss–Bonnet Gravities

Quantum corrections to the thermodynamics of rotating charged BTZ black hole in gravity's rainbow

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