  We present BeppoSAX observations of the Seyfert 1.8 galaxy NGC1365 in the
0.1--100 keV range. The source was 6 times brighter than during an ASCA
observation 3 years earlier. The 4--10 keV flux is highly variable during the
BeppoSAX observation, while the soft (0.1-4 keV) emission is constant within
the errors. Both a cold and a warm reflector and a cold absorber are required
to explain the observed spectrum. The comparison between ASCA and BeppoSAX
spectra strongly suggests that the circumnuclear material has a more complex
structure than a simple homogeneous torus, with quite different absorbing gas
columns along different lines of sight. A broad iron K_alpha line is also
present in the spectrum, with the peak energy significantly redshifted. This
can be explained by means of a relativistic disk line model. Alternatively, a
warm absorption Fe line system with N_H ~ 10^23 cm^(-2) could account for the
observed line profile.
