  The enigmatic type IIP SN 2016X demonstrates the unprecedented asphericity in
the nebular H-alpha line profile, the absence of nebular [O I] emission, and
the unusual occultation effect due to the internal dust. The hydrodynamic
modelling of the bolometric light curve and expansion velocities suggests that
the event is an outcome of the massive star explosion that ejected 28 Msun with
the kinetic energy of 1.7x10^51 erg and 0.03 Msun of radioactive Ni-56. We
recover the bipolar distribution of Ni-56 from the H-alpha profile via the
simulation of the emissivity produced by non-spherical Ni-56 ejecta. The
conspicuous effect of the dust absorption in the H-alpha profile rules out the
occultation by the dusty sphere or dusty thick disk but turns out consistent
with the thin dusty disk-like structure in the plane perpendicular to the
bipolar axis. We speculate that the absence of the nebular [O I] emission might
originate from the significant cooling of the oxygen-rich matter mediated by CO
and SiO molecules.
