  The study of a disturbed accretion disk holds great significance in the realm
of astrophysics, as such events play a crucial role in revealing the nature of
disk structure, the release of energy, and the generation of shock waves.
Consequently, they can help explain the causes of X-ray emissions observed in
black hole accretion disk systems. In this paper, we perturb the stable disk
formed by spherical accretion around Kerr and EGB black holes. This
perturbation reveals one- and two-armed spiral shock waves around the black
hole. We find a strong connection between these waves and the black hole spin
parameter (a/M) and the EGB coupling constant (\alpha). Specifically, we found
that as \alpha increases in the negative direction, the dynamics of the disk
and the waves become more chaotic. Additionally, we observe that the angular
momentum of the perturbing matter significantly affects mass accretion and the
oscillation of the arising shock waves. This allows us to observe changes in
QPO frequencies. Particularly, perturbations with angular momentum matching the
observed $C-$ type low-frequency QPOs of the GRS 1915 + 105 source. Thus, we
conclude that the possibility of the occurrence of shock waves within the
vicinity of GRS 1915 + 105 is substantial.
