  The ability of bumblebee gravity models to explain dark energy, which is the
phenomenon responsible for the universe's observed accelerated expansion, is
one of their most significant applications. An effect that causes faster
expansion can be linked to how much the Lorentz symmetry of our universe is
violated. Moreover, since we do not know what generates dark energy, the
bumblebee gravity theory seems highly plausible. By utilizing the physical
changes happening around a rotating bumblebee black hole (RBBH), we aim to
obtain more specific details about the bumblebee black hole's spacetime and our
universe. However, as researched in the literature, slow-spinning RBBH (SRBBH)
spacetime, which has a higher accuracy, will be considered instead of general
RBBH. To this end, we first employ the Rindler--Ishak method (RIM), which
enables us to study how light is bent in the vicinity of a gravitational lens.
We evaluate the deflection angle of null geodesics in the equatorial plane of
the SRBBH spacetime. Then, we use astrophysical data to see the effect of the
Lorentz symmetry breaking (LSB) parameter on the bending angle of light for
numerous astrophysical stars and black holes. We also acquire the analytical
greybody factors (GFs) and quasinormal modes (QNMs) of the SRBBH. Finally, we
visualize and discuss the results obtained in the conclusion section.
