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

¹ Institut d’Astrophysique de Paris, CNRS-Sorbonne Université, 98 bis boulevard Arago, 75014 Paris, France
e-mail: dessart@iap.fr
² Department of Physics and Astronomy & Pittsburgh Particle Physics, Astrophysics, and Cosmology Center (PITT PACC), University of Pittsburgh, 3941 O’Hara Street, Pittsburgh, PA 15260, USA
³ Tuorla Observatory, Department of Physics and Astronomy, 20014 University of Turku, Finland
⁴ Finnish Centre for Astronomy with ESO (FINCA), 20014 University of Turku, Finland

Received: 14 October 2021
Accepted: 26 November 2021

Abstract

Type Ibn supernovae (SNe) are a mysterious class of transients whose spectra exhibit persistently narrow He I 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 a peak luminosity of a few 10⁴⁴ erg s⁻¹ on day timescales, which is reminiscent of exceptional events such as AT 2018cow. 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 ∼10⁴³ erg s⁻¹. 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 M_⊙ helium star, most likely arising from interacting binaries and colliding with a massive helium-rich, probably ejecta-like, CSM at ∼10¹⁵ 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 such as 2006jc, 2011hw, or 2018bcc at late times and suggest a composition made of about 50% helium, a solar metallicity, and a total ejecta and CSM mass of 1–2 M_⊙. A lower fractional helium abundance leads to weak or absent He I lines and thus excludes more massive configurations for observed Type Ibn SNe. Further, the dominance of Fe II emission below 5500 Å seen in Type Ibn SNe at late times is not predicted at low metallicity. Hence, despite their promising properties, Type Ibn SNe from a pulsational-pair instability in very massive stars, requiring low metallicity, probably have not been observed yet.