Helium stars exploding in circumstellar material and the origin of Type Ibn supernovae

TL;DR

This paper investigates the explosion mechanisms and spectral features of Type Ibn supernovae through radiation-hydrodynamics and radiative-transfer simulations, revealing their likely origins from low-energy helium star explosions interacting with dense circumstellar material.

Contribution

It provides the first detailed modeling of Type Ibn supernovae spectra and light curves, linking their properties to low-energy helium star explosions in binary systems with dense CSM.

Findings

Standard helium-star explosions in dense CSM can produce luminous peaks similar to AT2018cow.

Most Type Ibn SNe likely originate from low-energy explosions of <~5 Msun helium stars.

Late-time spectra suggest a composition of about 50% helium and total ejecta/CSM mass of 1-2 Msun.

Abstract

Type Ibn supernovae (SNe) are a mysterious class of transients whose spectra exhibit persistently narrow HeI lines, and whose bolometric light curves are typically fast evolving and overluminous at peak relative to standard Type Ibc SNe. We explore the interaction scenario of such Type Ibn SNe by performing radiation-hydrodynamics and radiative-transfer calculations. We find that standard-energy helium-star explosions within dense wind-like circumstellar material (CSM) can reach on day timescales a peak luminosity of a few 10^44 erg/s, reminiscent of exceptional events like AT2018cow. Similar interactions but with weaker winds can lead to Type Ibc SNe with double-peak light curves and peak luminosities in the range ~10^42.2 to ~10^43 erg/s. In contrast, the narrow spectral lines and modest peak luminosities of most Type Ibn SNe are suggestive of a low-energy explosion in an initially <~5 Msun helium star, most likely arising from interacting binaries, and colliding with a massive helium-rich, probably ejecta-like, CSM at ~10^15 cm. Nonlocal thermodynamic equilibrium radiative-transfer simulations of a slow-moving dense shell born out and powered by the interaction compare favorably to Type Ibn SNe like 2006jc, 2011hw, or 2018bcc at late times and suggest a composition made of about 50% helium, a solar metallicity, and a total ejecta/CSM mass of 1-2Msun. A lower fractional helium abundance leads to weak or absent HeI lines and thus excludes more massive configurations for observed Type Ibn SNe. Further, the dominance of FeII emission below 5500A seen in Type Ibn SNe at late times is not predicted at low metallicity. Hence, despite their promising properties, Type Ibn SNe from pulsational-pair instability in very massive stars, which requires low metallicity, have probably not yet been observed.