Constraints on charged black hole parameters using quasiperiodic oscillations data

被引：24

作者：

Rayimbaev, Javlon ^{[1
,2
,3
,4
]}

Ahmedov, Bobomurat ^{[1
,3
,5
]}

Bokhari, Ashfaque H. ^{[6
]}

机构：

[1] Ulugh Beg Astron Inst, Astron St 33, Tashkent 100052, Uzbekistan

[2] Akfa Univ, Kichik Halqa Yuli St 17, Tashkent 100095, Uzbekistan

[3] Natl Univ Uzbekistan, Tashkent 100174, Uzbekistan

[4] Tashkent State Tech Univ, Tashkent 100095, Uzbekistan

[5] Natl Res Univ TIIAME, Inst Fundamental & Appl Res, Kori Niyoziy 39, Tashkent 100000, Uzbekistan

[6] King Fahd Univ Petr & Minerals KFUPM, Dept Math, Coll Comp & Math, POB 31261, Dhahran 31262, Saudi Arabia

来源：

INTERNATIONAL JOURNAL OF MODERN PHYSICS D | 2022年 / 31卷 / 11期

关键词：

Charged black holes; quasiperiodic oscillations; microquasars; X-RAY BINARIES; KHZ QPOS; MASS; MODEL; FIELD; GRAVITATION; FREQUENCIES; PRECESSION; ORBITS; ENERGY;

D O I：

10.1142/S0218271822400041

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Testing gravity theories and constraining their parameters using data from astrophysical observations of quasiperiodic oscillations (QPOs) is a powerful approach to study the features of black holes (ills) and gravity theories in the strong field regime. To this end, we investigate the dynamics of the test particles in the vicinity of some charged BHs such as Reissner-Nordstrom (RN), regular Bardeen and Ayon-Beato-Garcia (ABG). In particular, we calculate harmonic oscillations and the innermost stable circular orbits (ISCOs) of test particles around these BHs. As an astrophysical application, we discuss the twin peak QPOs in relativistic precession (RP) model and give the possible values of the upper and lower frequencies of the QPOs at. the distance from ISCO to infinity around the extremely charged BHs. Moreover, we also investigate the position of the orbit, where twin peak QPO may take place around central (charged) BH in the microquasar GRS 1915-105. We also study the dependence of the distance between the QPO position and ISCO from the BH charge. Using the upper and lower frequencies of the QPO, we obtain the relationship between the mass and charge of the central BH in the microquasar. Finally, we compare the effects of the spin of the Kerr BH and BH charges on the QPO in microquasar GRS 1915-105. We find that the BH charge can mimic the spin up to a/M = 0.2927 in the Bardeen model and up to a/M = 0.7687 in the case of special regular BH, admitting the same QPO frequencies.

引用

页数：20

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