2021
DOI: 10.3847/1538-4357/ac2c63
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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 timesc… Show more

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Cited by 13 publications
(14 citation statements)
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References 59 publications
(87 reference statements)
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“…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).…”
Section: Introductionmentioning
confidence: 99%
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“…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).…”
Section: Introductionmentioning
confidence: 99%
“…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.…”
Section: Introductionmentioning
confidence: 99%
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“…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.…”
Section: Introductionmentioning
confidence: 94%
“…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.…”
Section: Metamorphosis From Type Ib To Type Iin and The Pre-sn Mass-l...mentioning
confidence: 99%