Wave-driven Mass Loss of Stripped Envelope Massive Stars: Progenitor-dependence, Mass Ejection, and Supernovae

Abstract

The discovery of rapidly rising and fading supernovae powered by circumstellar interaction has suggested the pre-supernova mass eruption phase as a critical phenomenon in massive star evolution. It is important to understand the mass and radial extent of the circumstellar medium (CSM) from theoretically predicted mass ejection mechanisms. In this work, we study the wave heating process in massive hydrogen-poor stars, running a suite of stellar models in order to predict the wave energy and pre-explosion timescale of surface energy deposition. We survey stellar models with main-sequence progenitor masses from 20–70 M ⊙ and metallicity from 0.002–0.02. Most of these models predict that less than ∼1047 erg is deposited in the envelope, with the majority of the energy deposited in the last week of stellar evolution. This translates to CSM masses less than ∼10−2 M ⊙ that extend to less than ∼1014 cm, too small to greatly impact the light curves or spectra of the subsequent supernovae, except perhaps during the shock breakout phase. However, a few models predict somewhat higher wave energy fluxes, for which we perform hydrodynamical simulations of the mass ejection process. Radiative transfer simulations of the subsequent supernovae predict a bright but brief shock-cooling phase that could be detected in some Type Ib/c supernovae if they are discovered within a couple days of explosion.

Wave-driven Outbursts and Variability of Low-mass Supernova Progenitors

“…While most models were unlikely to produce observable pre-SN outbursts, the lowest-and highestmass stars experienced the highest levels of wave heating and were favored to drive outbursts. Leung et al (2021) surveyed the upper end of this mass range with the updated physics, extending up to M ZAMS = 70 M e and including hydrogen-poor stars, and likewise predicted less energy deposited in the envelope and less mass loss than prior work. Their hydrodynamical simulations of the most energetic high-mass model ejected at most 0.01 M e of material close to core collapse, forming quite confined CSM.…”

Eruption of the Envelope of Massive Stars by Energy Injection with Finite Duration

“…Woosley et al (2007) proposed pulsational pair instability arising from the production of electron-positron pairs in the core of very massive stars. Finally, wave-driven mass loss sourced by nuclear burning in the core is also proposed (e.g., Quataert & Shiode 2012;Shiode & Quataert 2014;Fuller 2017;Fuller & Ro 2018;Leung & Fuller 2020; Leung et al 2021aLeung et al , 2021bWu & Fuller 2021).…”

“…Modelings of continuous energy injection onto the stellar envelope were recently considered by several works (Leung & Fuller 2020;Leung et al 2021aLeung et al , 2021b, in the context of wave-driven mass loss. In Leung & Fuller (2020), the amount and asymmetry of the mass loss was investigated by twodimensional hydrodynamic simulations of hydrogen-rich progenitors.…”

“…This work focused on parameterizing the energy injection onto a hydrogen-poor progenitor in order to reproduce the specific Type Ic SN 2018gep. Leung et al (2021b) improved the modeling of wave heating and investigated the mass loss, but this work also focused on hydrogen-poor progenitors which are irrelevant to SNe IIn. Moreover, common to these works is that the specific conditions necessary for mass loss to occur were not calculated.…”

An environmental analysis of the Type Ib SN 2019yvr and the possible presence of an inflated binary companion

“…It is not yet fully clear what physical mechanism(s) drives the SN progenitors' enhanced mass-loss just before their core collapse. Current models include, to name a few, conv ection-e xcited wav e heating (Quataert & Shiode 2012 ;Shiode & Quataert 2014 ;Fuller 2017 ;Fuller & Ro 2018 ;Leung, Wu & Fuller 2021 ;, continuum-driven super-Eddington winds (Ofek et al 2016 ), hydrodynamical instabilities at late nuclear burning stages (Smith & Arnett 2014 ), and binary merger (Che v alier 2012 ). Margutti et al ( 2017 ) also proposed that 3.8-10 per cent of Type Ib/c SN progenitors can e xperience v ery late Case-C common-env elope evolution, which can efficiently eject dense CSM without the need to invoke an extra eruption from the progenitor.…”