Supernova-induced Binary-interaction-powered Supernovae: A Model for SN2022jli

Abstract We present 3D hydrodynamical modelling of supernova (SN)-induced binary-interaction-powered SNe; a scenario proposed for the peculiar type Ic SN SN2022jli. In this scenario, SN ejecta of a stripped-envelope star impact a close-by stellar companion, temporarily inflating the envelope. The expanded envelope engulfs the neutron star (NS), causing strong mass accretion at super-Eddington rates. Feedback from the accretion powers the SN light curve with periodic undulations. Our simulations capture key features of SN2022jli, both the overall decline and the superimposed undulations of the light curve. Based on our parameter study, we find that (i) the accretion feedback should be sufficiently geometrically confined and (ii) the eccentricity of the post-SN binary orbit should be 0.8 ≲ e ≲ 0.9 to sustain a high accretion rate and match the low undulation amplitude (Δ L / L ∼ 0.1) of SN2022jli. Different combinations of parameters could account for other SNe like SN2022mop, SN2009ip and SN2015ap, which have varying undulation periods and amplitudes. We also discuss possible explanations for other key features of SN2022jli such as the γ -ray detection at ∼200 days and the rapid optical drop at ∼250 days. Finally, we speculate on the future evolution of the system and its relation to existing NS binaries.