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We use the two-components bipolar toy model of core collapse supernova (CCSN)ejecta to fit the rapid decline from maximum luminosity in the light curve ofthe type IIb CCSN SN 2018gk (ASASSN-18am). In this toy model we use a templatelight curve from a different CCSN that is similar to SN 2018gk, but that has norapid drop in its light curve. The bipolar morphology that we model with apolar ejecta and an equatorial ejecta increases the maximum luminosity andcauses a steeper decline for an equatorial observer, relative to a similarspherical explosion. The total energy and mass of our toy model for SN 2018gkare E=5e51 erg and M=2.7Mo. This explosion energy is more than what aneutrino-driven explosion mechanism can supply, implying that jets exploded SN2018gk. These energetic jets likely shaped the ejecta to a bipolar morphology,as our toy model requires. We crudely estimate that f=2-5% of all CCSNe showthis behavior, most being hydrogen deficient (stripped-envelope) CCSNe, as weobserve them from the equatorial plane. We estimate the overall fraction ofCCSNe that have a pronounced bipolar morphology to be 5-15% of all CCSNe.

Modelling light curves of bipolar core collapse supernovae from the equatorial plane