  RXCJ0232.2-4420, at $z$ = 0.28, is a peculiar system hosting a radio halo
source around the cool-core of the cluster. To investigate its formation and
nature, we used archival {\it Chandra} and XMM-\textit{Newton} X-ray data to
study the dynamical state of the cluster and detect possible substructures in
the hot gas. Its X-ray surface brightness distribution shows no clear
disruption except an elongation in the North-East to South-West direction. We
perform the unsharp masking technique and compute morphology parameters (Gini,
$M_{20}$ and concentration) to characterise the degree of disturbance in the
projected X-ray emission. Both of these methods revealed a substructure, which
is located at $\sim$ 1$'$ from the cluster core in the South-West direction.
Previous spectral analysis conducted for RXCJ0232.2-4420 concluded that there
are a short cooling time and low entropy at the cluster centre, indicating that
the cluster has a cool core. Thus, we suggest that RXCJ0232.2-4420 may be a
system where the core of the cluster is not showing any sign of disturbance,
but the South-West substructure could be pumping energy to the detected radio
halo via turbulence.
