A one-zone radioactive heating model with macroscopic nickel-oxygen mixing reproduces the [O III] luminosity of SN 2018ibb and yields a scaling relation for line strength among PISNe.
PISN 2018ibb: radioactive emission of [O III] lines
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abstract
Supernova 2018ibb of the PISN category related to the dynamical instability of oxygen core in a supermassive star induced by pair-creation shows at the nebular stage strong [\oiii] emission lines of an uncertain origin. I propose a simple model that demonstrates a possibility of [O III] lines emission from the supernova oxygen matter ionized and heated by the $^{56}$Co radioactive decay. The reason is pinpointed by which the [O III] line luminosity among supernovae of PISN category can vary in a broad range.
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PISN 2018ibb: radioactive emission of [O III] lines
A one-zone radioactive heating model with macroscopic nickel-oxygen mixing reproduces the [O III] luminosity of SN 2018ibb and yields a scaling relation for line strength among PISNe.