Magnetized Particle Motion in γ-Spacetime in a Magnetic Field

Abdujabbarov, Ahmadjon; Rayimbaev, Javlon; Atamurotov, Farruh; Ahmedov, Bobomurat

doi:10.3390/galaxies8040076

Cited by 28 publications

(8 citation statements)

References 94 publications

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“…However, in order to tell an astrophysical black hole to be either spinning or not, a technique of X-ray reflection spectroscopy is quite effective [46]. Many astrophysical black holes are modelled using Kerr black hole or Kerr-like black holes in the modified gravity theories [40,47,48,49,50], however static and spherically symmetric black holes in different modified gravity theories may still be used as model for astrophysical black holes due to their simplicity. In such cases, the astrophysical effects of black hole spin on particle motion may also mimic the effects due to modified gravity.…”

Section: Astrophysical Applications: Bk Bh Vs Kerr Bhmentioning

confidence: 99%

Quasiperiodic Oscillations, Quasinormal Modes and Shadows of Bardeen-Kiselev Black Holes

Rayimbaev,

Majeed,

Jamil

et al. 2022

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In this article, we study the particle dynamics around a static and spherically symmetric Bardeen-Kiselev black hole (BK BH) which is a solution of the Einstein-non-linear Maxwell field equations along with a quintessential field. We discuss its essential geometrical properties such as scalar invariants and size of innermost stable circular orbits. Dynamics of test particles around the BH is also studied. Moreover, we also computed the fundamental frequencies of a test particle orbiting the BH in a slightly perturbed orbit. Further, the degeneracy relations between the spin of rotating Kerr BH and magnetic charge of the BK BH at the values of the quintessential parameter ω q = −1/3 and in terms of the same values of innermost stable circular orbits (ISCOs) radius, energy efficiency, twin-peaks quasiperiodic oscillations (QPOs) frequencies and impact parameter for photon are also discussed in detail. Finally, we have investigated the relationship between the shadow radius and the real part of the quasinormal mode (QNM) frequency.

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Section: Astrophysical Applications: Bk Bh Vs Kerr Bhmentioning

confidence: 99%

Quasiperiodic Oscillations, Quasinormal Modes and Shadows of Bardeen-Kiselev Black Holes

Rayimbaev,

Majeed,

Jamil

et al. 2022

Preprint

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“…In theoretical studies and astrophysical measurements of ISCO radius of test particles, a problem of indistinguishability of different gravity effects may appear. In most cases BHs are considered as rotational Kerr BHs, however, other some types of static BHs can provide similar gravitational effects on ISCO radius as rotating BH [66][67][68][69]. In such cases, it is quite difficult to distinguish the difference of gravitational effects of the two different types of BHs.…”

Section: Regular Mog Bh Versus Kerr Bh: the Same Iscomentioning

confidence: 99%

Dynamics of Test Particles and Twin Peaks QPOs around Regular Black Holes in Modified Gravity

et al. 2021

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In this work, we have presented a detailed analysis of the event horizon of regular black holes (BHs) in modified gravity known as MOG, the so-called regular MOG BH. The motion of neutral particles around the BH has also been explored. The test particle motion study shows that the positive (negative) values of the MOG parameter mimic the spin of a rotating Kerr BH, providing the same values for the innermost stable pro-grade (retrograde) orbits of the particles in the range of the spin parameter a/M∈(−0.4125,0.6946). The efficiency of energy release from the accretion disk by the Novikov–Thorne model has been calculated, and the efficiency was shown to be linearly proportional to the increase of the MOG parameter α. Moreover, we have developed a new methodology to test gravity theories in strong-field regimes using precision data from twin-peaked quasiperiodic oscillations (QPOs) of objects calculating possible values of upper and lower frequencies. However, it is obtained that the positive MOG parameter can not mimic the spin of Kerr BHs in terms of the same QPO frequencies. We have provided possible ranges for upper and lower frequencies of twin-peak QPOs with the ratio of the upper and lower frequencies of 3:2 around regular MOG BHs in the different models. Moreover, as an example, we provide detailed numerical analysis of the QPO of GRS 1915+105 with the frequencies νU=168±5Hz and νL=113±3Hz. It is shown that the central BH of the QPO object can be a regular MOG BH when the value of the parameter is α=0.2844−0.1317+0.0074 and shines in the orbits located at the distance r/M=7.6322−0.0826+0.0768 from the central BH. It is also shown that the orbits where QPOs shine are located near the innermost stable circular orbit (ISCO) of the test particle. The correlation between the radii of ISCO and the QPO orbits is found, and it can be used as a new theoretical way to determine ISCO radius through observational data from the QPOs around various compact objects.

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“…The dynamics of particles with the intrinsic non-zero dipolar magnetic field around non-rotating and rotating black holes immersed in an external magnetic field have been studied in [48,49]. Our recent work was devoted to a study of the magnetized particle motion around an RN black hole in a magnetic field in different gravity models and theories [50][51][52][53][54][55][56][57][58][59][60][61]. The electromagnetic field properties and its influence on particle dynamics have been explored in Refs.…”

Section: Introductionmentioning

confidence: 99%

Distinguishing magnetically and electrically charged Reissner–Nordström black holes by magnetized particle motion

et al. 2021

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In the present paper, we investigate the dynamics of magnetized particles around magnetically and electrically Reissner–Nordström (RN) black hole. The main idea of the work is to distinguish the effects of electric and magnetic charges of the RN black hole and spin of the rotating Kerr black hole through the dynamics of the magnetized particles. In this study, we have treated a magnetized neutron star as a magnetized test particle, in particular, the magnetar SGR (PSR) J1745-2900 orbiting around the supermassive black hole Sagittarius A* (SMBH SgrA*) with the magnetic interaction parameter $$b=0.716$$ b = 0.716 and the parameter $$\beta =10.2$$ β = 10.2 . The comparison of the effects of the magnetic and electric charges, and magnetic interaction parameters on the dynamics of the magnetar modeled as a magnetized particle near the SMBH Sgr A* has shown that the magnetic charge of the RN black hole can mimic the spin parameter of a rotating Kerr black hole up to $$a/M \simeq 0.82$$ a / M ≃ 0.82 . The external magnetic field can mimic the magnetic charge of the RN black hole up to $$Q_m/M=0.4465$$ Q m / M = 0.4465 . We have shown that the electric charge of the RN black hole can mimic the black hole magnetic charge up to $$Q_m/M=0.5482$$ Q m / M = 0.5482 and the magnetic field interaction with the magnetized particle acts against the increase of the mimicking value of the black hole spin parameter. The studies may be helpful to explain the observability of radio pulsars around the SMBH SgrA* system and taking it as a real astrophysical laboratory to get more precise constraints on the central black hole and dominated parameters of the alternate gravity. Finally, we have investigated the effects of magnetic and electric charge of the RN black hole in the center-of-mass energy of head-on collisions of magnetized particles with neutral, electrically charged, and magnetized particles. Both electric and magnetic charges of the RN black hole would lead to an increase in the center of the mass–energy of the collisions.

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Magnetized Particle Motion in γ-Spacetime in a Magnetic Field

Cited by 28 publications

References 94 publications

Quasiperiodic Oscillations, Quasinormal Modes and Shadows of Bardeen-Kiselev Black Holes

Quasiperiodic Oscillations, Quasinormal Modes and Shadows of Bardeen-Kiselev Black Holes

Dynamics of Test Particles and Twin Peaks QPOs around Regular Black Holes in Modified Gravity

Distinguishing magnetically and electrically charged Reissner–Nordström black holes by magnetized particle motion

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