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The unusual Type IIP SN 2017gmr is revisited in order to pinpoint the originof its anomalous features, including the peculiar light curve after about 100days. The hydrodynamic modelling suggests the enormous explosion energy ofabout 10^52 erg. We find that the light curve with the prolonged plateau/tailtransition can be reproduced either in the model with a high hydrogen abundancein the inner ejecta and a large amount of radioactive Ni-56, or in the modelwith an additional central energy source associated with the fallback/magnetarinteraction in the propeller regime. The asymmetry of the late H-alpha emissionand the reported linear polarization are reproduced by the model of the bipolarNi-56 ejecta. The similar bipolar structure of the oxygen distribution isresponsible for the two-horn structure of the [O I] 6360, 6364 A emission. Thebipolar Ni-56 structure along with the high explosion energy are indicative ofthe magneto-rotational explosion. We identify narrow high-velocity absorptionfeatures in H-alpha and He I 10830 A lines with their origin in the fragmentedcold dense shell formed due to the outer ejecta deceleration in a confinedcircumstellar shell.

Enormous explosion energy of Type IIP SN 2017gmr with bipolar Ni-56 ejecta