The hard X-ray properties of the Seyfert nucleus in NGC 1365

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 obser vation 3 years earlier. The 4-10 keV flux is highly variable during the Bep poSAX observation, while the soft (0.1-4 keV) emission is constant within t he errors. Both a cold and a warm reflector and a cold absorber are require d to explain the observed spectrum. The comparison between ASCA and BeppoSA X spectra strongly suggests that the circumnuclear material has a more comp lex structure than a simple homogeneous torus, with quite different absorbi ng gas columns along different lines of sight. A broad iron K alpha line is also present in the spectrum, with the peak energy significantly redshifte d. This can be explained by means of a relativistic disk line model. Altern atively, a warm absorption Fe line system with N-H similar or equal to 10(2 3) cm(-2) could account for the observed line profile.