  The rotating loop quantum gravity black hole is a newly proposed non-singular
black hole, which eliminates spacetime singularities when a regularization
parameter is introduced through loop quantum corrections. This parameter is
expected to give rise to observable effects. In this paper, the dynamical
behavior of a scalar field near a rotating loop quantum gravity black hole is
investigated. Given a small initial perturbation, we obtain the waveform of
massless scalar fields evolving over time. By analyzing the waveform, we find
that the regularization parameter only affects the damping oscillation of
waveform, but not the initial outburst and late-time tail stages. This behavior
is characterized by quasi-normal modes. Under scalar field perturbations, the
loop quantum black holes remain stable. Moreover, we calculate the quasi-normal
modes of massive scalar fields by three numerical methods, which are the Prony,
WKB, and shooting methods, respectively. Our results indicate that the real
part of quasi-normal modes depends only on the regularization parameter, while
the imaginary part does not only on the regularization parameter but also on
the angular momentum. Finally, we study the amplification effect of rotating
black holes, i.e., the superradiance. Our analyses indicate the existence of
stronger superradiance around loop quantum gravity black holes compared to Kerr
ones.
