SN 1994W: An Interacting Supernova or Two Interacting Shells?

TL;DR

This study provides a detailed spectroscopic analysis of SN 1994W, suggesting it may result from shell interactions rather than a typical core-collapse supernova, highlighting unique radiation sources and scattering mechanisms.

Contribution

It offers a novel interpretation of SN 1994W's spectral features, proposing a shell interaction model without core collapse and explaining line profiles through electron scattering.

Findings

Optically-thick photosphere explains line profiles without external shells.

Slow expansion allows electron scattering to produce broad wings.

Low 56Ni yields suggest a non-standard supernova origin.

Abstract

We present a multi-epoch quantitative spectroscopic analysis of the Type IIn SN 1994W, an event interpreted by Chugai et al. as stemming from the interaction between the ejecta of a SN and a 0.4Msun circumstellar shell ejected 1.5yr before core collapse. During the brightening phase, our models suggest that the source of optical radiation is not unique, perhaps associated with an inner optically-thick Cold Dense Shell (CDS) and outer optically-thin shocked material. During the fading phase, our models support a single source of radiation, an hydrogen-rich optically-thick layer with a near-constant temperature of ~7000K that recedes from a radius of 4.3x10^15 at peak to 2.3x10^15cm 40 days later. We reproduce the hybrid narrow-core broad-wing line profile shapes of SN 1994W at all times, invoking an optically-thick photosphere exclusively (i.e., without any external optically-thick shell). In SN 1994W, slow expansion makes scattering with thermal electrons a key escape mechanism for photons trapped in optically-thick line cores, and allows the resulting broad incoherent electron-scattering wings to be seen around narrow line cores. In SNe with larger expansion velocities, the thermal broadening due to incoherent scattering is masked by the broad profile and the dominant frequency redshift occasioned by bulk motions. Given the absence of broad lines at all times and the very low 56Ni yields, we speculate whether SN 1994W could have resulted from an interaction between two ejected shells without core collapse. The high conversion efficiency of kinetic to thermal energy may not require a SN-like energy budget for SN1994W.