Distinguishing signature of Kerr-MOG black hole and superspinar via Lense–Thirring precession

Parthapratim Pradhan

doi:10.1140/epjc/s10052-024-13210-w

2024 Impact factor 4.8

Particles and Fields

Open Access

Eur. Phys. J. C (2024) 84: 841
https://doi.org/10.1140/epjc/s10052-024-13210-w

Regular Article – Theoretical Physics

Distinguishing signature of Kerr-MOG black hole and superspinar via Lense–Thirring precession

Parthapratim Pradhan^a

Department of Physics, Hiralal Mazumdar Memorial College for Women, 700035, Dakshineswar, Kolkata, India

^a pppradhan77@gmail.com

Received: 17 June 2024
Accepted: 4 August 2024
Published online: 21 August 2024

Abstract

We examine the geometrical differences between the black hole (BH) and naked singularity (NS) or superspinar via Lense–Thirring (LT) precession in spinning modified-gravity (MOG). For BH case, we show that the LT precession frequency ( $Ω_{LT}$ $\Omega _{LT}$ ) along the pole is proportional to the angular-momentum (J) parameter or spin parameter (a) and is inversely proportional to the cubic value of radial distance parameter, and also governed by Eq. (1). Along the equatorial plane it is governed by Eq. (2). While for superspinar, we show that the LT precession frequency is inversely proportional to the cubic value of the spin parameter and it decreases with distance by MOG parameter as derived in Eq. (3) at the pole and in the limit $a > > r$ $$a>>r$$ (where a is spin parameter). For $θ \neq \frac{π}{2}$ $\theta \ne \frac{\pi }{2}$ and in the superspinar limit, the spin frequency varies as $Ω_{LT} \propto \frac{1}{a^{3} {cos}^{4} θ}$ $\Omega _{LT}\propto \frac{1}{a^3\cos ^4\theta }$ and by Eq. (38).

© The Author(s) 2024

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