  [ABRIDGED] Stellar feedback in high-redshift galaxies plays an important role
in the re-ionization epoch of the Universe. Green Pea galaxies (GPs) postulate
as favorite local laboratories. However, at their typical redshift of
$z\sim0.2$, the most intimate interaction between stars and surrounding ISM
cannot be disentangled. Detailed studies of Blue Compact Dwarf galaxies (BCDs)
are necessary to anchor our investigations on them. We present here a study in
detail UM 462, a BCD with similar properties to GPs uisng high quality optical
IFS data with MUSE. Total oxygen abundance by means of the direct method is
12+$\log$(O/H)$\sim$8.02 and homogenous all over the galaxy, in stark contrast
with the metallicities derived from several strong line methods. The velocity
field for the ionised gas presents a velocity stratification in the area
towards the north with redder velocities in the high ionisation lines and bluer
velocities in the low ionisation lines. This is the only area with velocity
dispersions clearly above the MUSE instrumental width, and it is surrounded by
two $\sim$1 kpc-long structures nicknamed \emph{the horns}. We interpret the
observational evidence in that area as a fragmented super-bubble fruit of the
stellar feedback and it may constitute a preferred channel for LyC photons from
the youngest generation of stars to escape. The most recent SF seems to
propagate from the outer to the inner parts of the galaxy, and then from east
to west. We identified a supernova remnant and Wolf-Rayet stars - as traced by
the red bump - that support this picture. The direction of the propagation
implies the presence of younger Wolf-Rayet stars at the maximum in H$\alpha$.
The ensemble of results exemplifies the potential of 2D detailed spectroscopic
studies of dwarf star-forming galaxies at high spatial resolution as key
reference for similar studies on primeval galaxies.
