Numerical models of collisions between core-collapse supernovae and circumstellar shells

TL;DR

This study uses numerical simulations to analyze how the properties of circumstellar shells influence the lightcurves of core-collapse supernovae, highlighting the dominant role of shell mass in luminosity and duration.

Contribution

It provides a detailed parameter study of supernova-shell interactions, emphasizing the impact of shell mass, velocity, and geometry on observable lightcurves, and offers diagnostic tools for interpreting observations.

Findings

Higher shell mass leads to higher peak luminosity.

Massive shells (>10 M_sun) sustain luminosity over 100 days.

Shell velocity and shape influence lightcurve features.

Abstract

Recent observations of luminous Type IIn supernovae (SNe) provide compelling evidence that massive circumstellar shells surround their progenitors. In this paper we investigate how the properties of such shells influence the SN lightcurve by conducting numerical simulations of the interaction between an expanding SN and a circumstellar shell ejected a few years prior to core collapse. Our parameter study explores how the emergent luminosity depends on a range of circumstellar shell masses, velocities, geometries, and wind mass-loss rates, as well as variations in the SN mass and energy. We find that the shell mass is the most important parameter, in the sense that higher shell masses (or higher ratios of M_shell/M_SN) lead to higher peak luminosities and higher efficiencies in converting shock energy into visual light. Lower mass shells can also cause high peak luminosities if the shell is slow or if the SN ejecta are very fast, but only for a short time. Sustaining a high luminosity for durations of more than 100 days requires massive circumstellar shells of order 10 M_sun or more. This reaffirms previous comparisons between pre-SN shells and shells produced by giant eruptions of luminous blue variables (LBVs), although the physical mechanism responsible for these outbursts remains uncertain. The lightcurve shape and observed shell velocity can help diagnose the approximate size and density of the circumstellar shell, and it may be possible to distinguish between spherical and bipolar shells with multi-wavelength lightcurves. These models are merely illustrative. One can, of course, achieve even higher luminosities and longer duration light curves from interaction by increasing the explosion energy and shell mass beyond values adopted here.