  Accretion dynamics in the forming of young stars is still object of debate
because of limitations in observations and modelling. Through scaled laboratory
experiments of collimated plasma accretion onto a solid in the presence of a
magnetic field, we open first window on this phenomenon by tracking, with
spatial and temporal resolution, the dynamics of the system and simultaneously
measuring multiband emissions. We observe in these experiments that matter,
upon impact, is laterally ejected from the solid surface, then refocused by the
magnetic field toward the incoming stream. Such ejected matter forms a plasma
shell that envelops the shocked core, reducing escaped X-ray emission. This
demonstrates one possible structure reconciling current discrepancies between
mass accretion rates derived from X-ray and optical observations.
