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We propose a mechanism to explain the low-frequency QPOs observed in X-raybinary systems and AGNs. To do this, we perturbed stable accretion disks aroundKerr and EGB black holes at different angular velocities, revealing thecharacteristics of shock waves and oscillations presented on the disk. Applyingthis perturbation to scenarios with different alpha values for EGB black holesand different spin parameters for Kerr black holes, we numerically observedchanges in the dynamic structure of the disk and oscillations. Through variousnumerical modeling, we found that the formation of one- and two-armed spiralshock waves on the disk serves as a mechanism for the generation of QPOs. Wecompared the QPOs obtained from numerical calculations with the low-frequencyQPOs observed in $X-$ray binary systems and AGN sources. We found that theresults obtained are highly consistent with observations. We observed that theshock mechanism on the disk, which leads to quasi-periodic oscillations,explains the X-ray binaries and AGNs studied in this article. As a result ofthe numerical findings, we find that QPOs are more strongly dependent on theEGB constant rather than the black hole's spin parameter However, wehighlighted that the primary impact on oscillations and QPOs is driven by theperturbation's angular velocity. According to the results obtained from themodels, it has been observed that the perturbation's asymptotic speed atV_{\infty}=0.2 is responsible for generating QPO frequencies independently ofthe black hole's spin parameter and the EGB coupling constant. Therefore, forthe moderate value of V_{\infty}, a two-armed spiral shock wave formed on thedisk is suggested as a decisive mechanism in explaining low-frequency QPOs.

Proposing a Physical Mechanism to Explain Various Observed Sources of QPOs by Simulating the Dynamics of Accretion Disks around the Black Holes