Related progenitor models for long-duration gamma ray bursts and Type Ic superluminous supernovae

TL;DR

This paper models the late evolution of rapidly rotating Wolf-Rayet stars to explore their potential as progenitors for long-duration gamma-ray bursts and Type Ic superluminous supernovae, highlighting the role of angular momentum and mass loss.

Contribution

It provides new models linking progenitor star properties to diverse explosive phenomena, emphasizing the impact of rotation and mass loss on supernova and gamma-ray burst outcomes.

Findings

Lower mass models can produce magnetar-driven superluminous supernovae.

Higher mass models retain enough angular momentum for long-duration gamma-ray bursts.

Massive models may undergo pulsational pair-instability, affecting supernova signatures.

Abstract

We model the late evolution and mass loss history of rapidly rotating Wolf-Rayet stars in the mass range $5\,\rm{M}_{\odot}\dots 100\,\rm{M}_{\odot}$. We find that quasi-chemically homogeneously evolving single stars computed with enhanced mixing retain very little or no helium and are compatible with Type\,Ic supernovae. The more efficient removal of core angular momentum and the expected smaller compact object mass in our lower mass models lead to core spins in the range suggested for magnetar driven superluminous supernovae. Our more massive models retain larger specific core angular momenta, expected for long-duration gamma-ray bursts in the collapsar scenario. Due to the absence of a significant He envelope, the rapidly increasing neutrino emission after core helium exhaustion leads to an accelerated contraction of the whole star, inducing a strong spin-up, and centrifugally driven mass loss at rates of up to $10^{-2}\,\rm{M}_{\odot}~\rm{yr^{-1}}$ in the last years to decades before core collapse. Since the angular momentum transport in our lower mass models enhances the envelope spin-up, they show the largest relative amounts of centrifugally enforced mass loss, i.e., up to 25\% of the expected ejecta mass. Our most massive models evolve into the pulsational pair-instability regime. We would thus expect signatures of interaction with a C/O-rich circumstellar medium for Type~Ic superluminous supernovae with ejecta masses below $\sim 10\,\rm{M}_{\odot}$ and for the most massive engine-driven explosions with ejecta masses above $\sim 30\,\rm{M}_{\odot}$. Signs of such interaction should be observable at early epochs of the supernova explosion, and may be related to bumps observed in the light curves of superluminous supernovae, or to the massive circumstellar CO-shell proposed for Type~Ic superluminous supernova Gaia16apd.