Ni Ejecta and Polarization in Type Iip Supernova 2004dj

I study a problem, whether the asymmetry of a 56 Ni ejecta that results in the asymmetry of the Hα emission line at the nebular epoch of the type IIP su-pernova SN 2004dj is able also to account for the recently detected polarization of the supernova radiation. I developed a model of the Hα profile and luminos-ity with a nonthermal ionization and excitation taken into account adopting an asymmetric bipolar 56 Ni distribution. On the background of the recovered distribution of the electron density I calculated the polarized radiation transfer. It is demonstrated that the observed polarization is reproduced at the nebular epoch around day 140 for the same parameters of the envelope and 56 Ni distribution for which the luminosity and profile of Hα are explained. Yet the model polarization decreases slower compared to observations. The origin of an additional component responsible for the early polarization on day 107 is discussed.