Supernova-induced binary-interaction-powered supernovae: a model for SN2022jli

TL;DR

This work investigates a SN-induced binary-interaction powering scenario for SN2022jli, proposing that a newborn neutron star accretes at super-Eddington rates from a heated companion envelope, thereby powering the observed light-curve features. Using 3D hydrodynamic simulations with SN-heating treated as energy injection and exploring accretion-feedback (none, thermal, bipolar), the authors reproduce the long-term decline and periodic undulations seen in SN2022jli for high orbital eccentricity ($e\gtrsim0.8$) and geometrically confined feedback, while showing that viewing angle and the exact accretion efficiency can modulate the observed amplitude. The model also offers explanations for late-time $\ ext{GeV}$ gamma-rays and H$\alpha$ emission, and constrains post-SN binary properties such as the periastron distance ($a_{\rm per}\lesssim 19R_\odot$). These results imply that SN-induced binary interactions could account for a class of peculiar transients and provide a framework to infer post-SN binary configurations from light curves, with implications for future LSST-era discoveries.

Abstract

We present 3D hydrodynamical modelling of supernova-induced binary-interaction-powered supernovae; a scenario proposed for the peculiar type Ic supernova SN2022jli. In this scenario, supernova ejecta of a stripped-envelope star impact a close-by stellar companion, temporarily inflating the envelope. The expanded envelope engulfs the neutron star, causing strong mass accretion at super-Eddington rates. Feedback from the accretion powers the supernova 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-supernova binary orbit should be $0.8\lesssim e\lesssim0.9$ to sustain a high accretion rate and match the low undulation amplitude ($ΔL/L\sim0.1$) of SN2022jli. Different combinations of parameters could account for other supernovae 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 $\sim200~\mathrm{d}$ and the rapid optical drop at $\sim250~\mathrm{d}$. Finally, we speculate on the future evolution of the system and its relation to existing neutron star binaries.

Figures (18)

• Figure 1: Animation of the 3D hydrodynamic simulations for the no feedback model (M05e05n). We show several different slices ($xy, xz, yz$), all cut through the centre of the companion star. The $z$ axis is the direction of the orbital angular momentum and the $x$ axis is aligned with the orbital major axis. The light blue dot marks the location of the point particle representing the ns. The animation runs from the start to end of our simulation ($\sim100~\mathrm{d}$). The static version displays four select snapshots from the second orbit.
• Figure 2: Same as Figure \ref{['fig:snapshots_nofeedback']} but for the thermal feedback model (M05e05t).
• Figure 3: Same as Figure \ref{['fig:snapshots_nofeedback']} but for the bipolar feedback model (M05e05b).
• Figure 4: Mass accretion rate evolution in our hydrodynamic simulations. We compare three different models with the same orbital parameters but different feedback methods: no feedback (model M05e05n; green), thermal feedback (model M05e05t; light green) and bipolar feedback (M05e05b; dark grey). Dashed vertical lines mark the periastron passage timings. For the no feedback model, we overplot the Bondi-Hoyle-Lyttleton accretion rate computed from Eq. (\ref{['eq:bondi']}) (dotted).
• Figure 5: Same as Figure \ref{['fig:mdot_feedback']} but comparing models with different companion masses: $M_2=3~M_\odot$ (model M03e05b; sky blue), $5~M_\odot$ (model M05e05b; dark grey) and $10~M_\odot$ (model M10e05b; blue). All models were simulated with bipolar feedback.