  A detailed understanding of a volcano inner structure is one of the
key-points for the volcanic hazards evaluation. To this aim, in the last
decade, geophysical radiography techniques using cosmic muon particles have
been proposed. By measuring the differential attenuation of the muon flux as a
function of the amount of rock crossed along different directions, it is
possible to determine the density distribution of the interior of a volcano. Up
to now, a number of experiments have been based on the detection of the muon
tracks crossing hodoscopes, made up of scintillators or nuclear emulsion
planes. Using telescopes based on the atmospheric Cherenkov imaging technique,
we propose a new approach to study the interior of volcanoes detecting the
Cherenkov light produced by relativistic cosmic-ray muons that survive after
crossing the volcano. The Cherenkov light produced along the muon path is
imaged as a typical annular pattern containing all the essential information to
reconstruct particle direction and energy. Our new approach offers the
advantage of a negligible background and an improved spatial resolution. To
test the feasibility of our new method, we have carried out simulations with a
toy-model based on the geometrical parameters of ASTRI SST-2M, i.e. the imaging
atmospheric Cherenkov telescope currently under installation onto the Etna
volcano. Comparing the results of our simulations with previous experiments
based on particle detectors, we gain at least a factor of 10 in sensitivity.
The result of this study shows that we resolve an empty cylinder with a radius
of about 100 m located inside a volcano in less than 4 days, which implies a
limit on the magma velocity of 5 m/h.
