  We present the first multidimensional, magnetohydrodynamic simulations which
capture the initial formation and the long-term sustainment of the enigmatic
coronal rain phenomenon. We demonstrate how thermal instability can induce a
spectacular display of in-situ forming blob-like condensations which then start
their intimate ballet on top of initially linear force-free arcades. Our
magnetic arcades host chromospheric, transition region, and coronal plasma.
Following coronal rain dynamics for over 80 minutes physical time, we collect
enough statistics to quantify blob widths, lengths, velocity distributions, and
other characteristics which directly match with modern observational knowledge.
Our virtual coronal rain displays the deformation of blobs into $V$-shaped like
features, interactions of blobs due to mostly pressure-mediated levitations,
and gives the first views on blobs which evaporate in situ, or get siphoned
over the apex of the background arcade. Our simulations pave the way for
systematic surveys of coronal rain showers in true multidimensional settings,
to connect parametrized heating prescriptions with rain statistics, ultimately
allowing to quantify the coronal heating input.
