2017MNRAS.472.5004U

We explore the well-observed Type IIP supernova 2013ej with peculiar luminosity evolution. It is found that the hydrodynamic model cannot reproduce in detail the bolometric luminosity at both the plateau and the radioactive tail. Yet the ejecta mass of 23-26 M_☉ and the kinetic energy of (1.2-1.4) x 10⁵¹ erg are determined rather confidently. We suggest that the controversy revealed in hydrodynamic simulations stems from the strong asphericity of the ⁵⁶Ni ejecta. An analysis of the asymmetric nebular H α line and of the peculiar radioactive tail made it possible to recover parameters of the asymmetric bipolar ⁵⁶Ni ejecta with the heavier jet residing in the rear hemisphere. The inferred ⁵⁶Ni mass is 0.039 M_☉, twice as large compared to a straightforward estimate from the bolometric luminosity at the early radioactive tail. The bulk of ejected ⁵⁶Ni has velocities in the range of 4000-6500 km s^–1. The linear polarization predicted by the model with the asymmetric ionization produced by bipolar ⁵⁶Ni ejecta is consistent with the observational value.