Eur. Phys. J. C (2025) 85: 780
https://doi.org/10.1140/epjc/s10052-025-14480-8

Regular Article - Theoretical Physics

Distinguishing between dark matter-black hole systems and naked singularities via quasi-periodic oscillations

College of Physics, Guizhou University, 550025, Guiyang, China

^a tangmr@gzu.edu.cn

Received: 2 March 2025
Accepted: 30 June 2025
Published online: 18 July 2025

Abstract

Quasi-Periodic Oscillations (QPOs) are an important phenomenon commonly observed in the X-ray radiation of black holes (BH) and neutron stars, closely related to the dynamics of accretion disks around Compact Objects (CO) and general relativistic effects. The objective of this study is to use the QPO phenomenon to distinguish between Dark Matter (DM)-BH systems and Naked Singularities (NS), as well as to investigate the effects of different dark matter models (Cold Dark Matter, CDM, and Scalar Field Dark Matter, SFDM) on the accretion disk dynamics. By introducing a DM correction model within the framework of general relativity, we systematically investigate the differences in dragging effects, characteristic frequency distribution, and the Innermost Stable Circular Orbit (ISCO) radius between DM-BH systems and NS, while analyzing the potential coupling between QPO frequencies and DM distribution. The main results of this study are as follows: In BH cases, the radial precession frequency ${\nu }_r$ is consistent with the High-Frequency QPO range only in the low-spin region ($a=0.1\sim 0.2$); the vertical precession frequency ${\nu }_{\theta }$ matches the Low-Frequency QPO range around $a=0.5$, while the nodal precession frequency ${\nu }_{\text{nod}}$ agrees with the Low-Frequency QPO range around $a=0.7$, and exhibits frequency reversal in the high-spin region ($0.7<a<1$). NS cases, however, display markedly different characteristics: both radial and vertical precession frequencies show monotonic decrease with significant amplification, with ${\nu }_r$ reaching kHz levels at $a=1\sim 1.2$, and ${\nu }_{\theta }$ reaching 700+ Hz at $a=1$, both far exceeding the QPO observational range; while the nodal precession frequency ${\nu }_{\text{nod}}$ remains consistently in the reverse state but with values falling within the High-Frequency QPO observational range. CDM and SFDM modulate the accretion disk dynamics at the order of ${10}^{-6}$.