Against the Wind: Radio Light Curves of Type Ia Supernovae Interacting with Low-Density Circumstellar Shells

TL;DR

This paper models the radio light curves of Type Ia supernovae interacting with low-density, finite-extent circumstellar shells, revealing sharply peaked signals and providing tools to infer CSM properties from observations.

Contribution

It introduces a new model for supernova interaction with finite shells, differing from the traditional continuous CSM assumption, and offers a method to deduce CSM characteristics from radio data.

Findings

CSM shells produce sharply peaked radio light curves.

Fiducial models follow a common evolution useful for analysis.

Application to SN 2011fe and SN 2014J non-detections demonstrates model utility.

Abstract

For decades, a wide variety of observations spanning the radio through optical and on to the x-ray have attempted to uncover signs of type Ia supernovae (SNe Ia) interacting with a circumstellar medium (CSM). The goal of these studies is to constrain the nature of the hypothesized SN Ia mass-donor companion. A continuous CSM is typically assumed when interpreting observations of interaction. However, while such models have been successfully applied to core-collapse SNe, the assumption of continuity may not be accurate for SNe Ia, as shells of CSM could be formed by pre-supernova eruptions (novae). In this work, we model the interaction of SNe with a spherical, low density, finite-extent CSM and create a suite of synthetic radio synchrotron light curves. We find that CSM shells produce sharply peaked light curves, and identify a fiducial set of models that all obey a common evolution and can be used to generate radio light curves for interaction with an arbitrary shell. The relations obeyed by the fiducial models can be used to deduce CSM properties from radio observations; we demonstrate this by applying them to the non-detections of SN 2011fe and SN 2014J. Finally, we explore a multiple shell CSM configuration and describe its more complicated dynamics and resultant radio light curves.