https://doi.org/10.1140/epjp/s13360-023-04283-9
Regular Article
Dynamics of spinning test particles around the Kerr–Newman–NUT black hole with quintessence in the Rastall gravity
1
New Uzbekistan University, Mustaqillik Avenue 54, 100007, Tashkent, Uzbekistan
2
Ulugh Beg Astronomical Institute, Astronomy St. 33, 100052, Tashkent, Uzbekistan
3
Institute of Nuclear Physics, Ulugbek 1, 100214, Tashkent, Uzbekistan
4
School of Physics and Astronomy, Shanghai Jiao Tong University, 800 Dongchuan Road, Minhang, 200240, Shanghai, People’s Republic of China
5
Shanghai Frontiers Science Center of Gravitational Wave Detection, 800 Dongchuan Road, Minhang, 200240, Shanghai, People’s Republic of China
6
School of Engineering, Central Asian University, 111221, Tashkent, Uzbekistan
7
Tashkent Institute of Irrigation and Agricultural Mechanization Engineers, Kori Niyoziy, 39, 100000, Tashkent, Uzbekistan
8
Samarkand State University, University Avenue 15, 140104, Samarkand, Uzbekistan
9
School of Electrical Engineering and Computer Science, National University of Sciences and Technology, H-12, Islamabad, Pakistan
10
Tashkent State Technical University, 100095, Tashkent, Uzbekistan
11
National University of Uzbekistan, 100174, Tashkent, Uzbekistan
12
Institute of Fundamental and Applied Research, National Research University TIIAME, Kori Niyoziy 39, 100000, Tashkent, Uzbekistan
d
ibrar.hussain@seecs.nust.edu.pk
Received:
3
May
2023
Accepted:
14
July
2023
Published online:
21
July
2023
This work is devoted to the study of motion of spinning test particles in the spacetime of the Kerr–Newman–NUT black hole with quintessence, in the Rastall gravity theory. We use the so-called Mathisson–Papapetrous–Dixon equation to investigate the dynamics of spinning test particles. We discuss the effect of the particle’s spin, s, and the spacetime parameters on the effective potential. Then, we focus on the innermost stable circular orbits (ISCOs) and show the dependence of the ISCO radius on the particle’s spin for different values of the metric parameters graphically. Then, we investigate the specific energy and the orbital angular momentum of the particle at the ISCO. Our results show that the black hole’s spin parameter a has an evident influence on the ISCO radius, followed by the quintessential parameter, 
, the quintessence state parameter, 
, and the Rastall gravity parameter, 
. We also discuss the constraint on the particle’s spin due to the superluminal bound for co-rotating and counter-rotating orbits, which changes depending on the values of the black hole’s parameters. Finally, we compare our results with the results for the Kerr black hole. We found that spacetime parameters increase the ISCO radius for co-rotating and counter-rotating circular orbits. Nevertheless, the energy at the ISCO is not affected strongly by the spacetime parameters for higher values of |s|.
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© The Author(s), under exclusive licence to Società Italiana di Fisica and Springer-Verlag GmbH Germany, part of Springer Nature 2023. Springer Nature or its licensor (e.g. a society or other partner) holds exclusive rights to this article under a publishing agreement with the author(s) or other rightsholder(s); author self-archiving of the accepted manuscript version of this article is solely governed by the terms of such publishing agreement and applicable law.
