  The phenomenon by which matter accumulates in the vicinity of a huge
celestial object is known as accretion. The gravitational energy is excreted as
a consequence of infalling matter onto compact objects. The accretion procedure
around celestial bodies like neutron stars, white dwarfs, and black holes has
considerable importance because of its ability to transform gravitational
energy into radiation. This study investigates the particle's geodesic motion
and accretion around the spherically symmetric Reissner-Nordstr\"{o}m black
hole coupled with a nonlinear electrodynamics field utilizing isothermal fluid.
The formation of the disc-like structure in the accretion process arises from
the geodesic motion exhibited by particles near the black hole. The circular
orbits, radiant flux energy, radioactive efficiency, and radiant temperature,
can be determined. Our study focuses on the examination of particles exhibiting
stable circular orbits within the equatorial plane. We analyze the
perturbations experienced by particles throughout employing restoring forces
and the oscillatory behavior of the particles around a compact object. We
conduct an analysis of the fluid's critical flow and maximum accretion rate.
Our results show how the black hole parameter $\zeta$ and charge $q$ affect the
circular geodesic of particles and the maximum accretion rate of the
Reissner-Nordstr\"{o}m black hole coupled with nonlinear electrodynamics.
