Pre-supernova outbursts via wave heating in massive stars – II. Hydrogen-poor stars

Fuller, Jim; Ro, Stephen

doi:10.1093/mnras/sty369

Cited by 125 publications

(157 citation statements)

References 81 publications

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“…We note that this condition is easily satisfied for a lower-mass progenitor star in an interacting binary system. Fuller & Ro (2018) also calculated this process in stars composed of a 5-M helium core evolved from a 15-M progenitor stripped of its hydrogen envelope. They found that wave heating can drive pre-SN eruptions with timescales and mass-loss rates consistent with observations.…”

Section: Mass Loss Mechanismsmentioning

confidence: 99%

Origins of Type Ibn SNe 2006jc/2015G in interacting binaries and implications for pre-SN eruptions

Sun

Maund

Hirai

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Type Ibn supernovae (SNe Ibn) are intriguing stellar explosions whose spectra exhibit narrow helium lines with little hydrogen. They trace the presence of circumstellar material (CSM) formed via pre-SN eruptions of their stripped-envelope progenitors. Early work has generally assumed that SNe Ibn come from massive Wolf-Rayet (WR) stars via single star evolution. In this paper, we report ultraviolet (UV) and optical observations of two nearby Type Ibn SNe 2006jc and 2015G conducted with the Hubble Space Telescope (HST) at late times. A point source is detected at the position of SN 2006jc, and we confirm the conclusion of Maund et al. that it is the progenitor's binary companion. Its position on the Hertzsprung-Russell (HR) diagram corresponds to a star that has evolved off the main sequence (MS); further analysis implies a low initial mass for the companion star (M 2 ≤ 12.3 +2.3 −1.5 M ) and a secondary-to-primary initial mass ratio very close to unity (q = M 2 /M 1 ∼ 1); the SN progenitor's hydrogen envelope had been stripped through binary interaction. We do not detect the binary companion of SN 2015G. For both SNe, the surrounding stellar populations have relatively old ages and argue against any massive WR stars as their progenitors. These results suggest that SNe Ibn may have lower-mass origins in interacting binaries. As a result, they also provide evidence that the giant eruptions commonly seen in massive luminous blue variables (LBVs) can also occur in much lower-mass, stripped-envelope stars just before core collapse.

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Section: Mass Loss Mechanismsmentioning

confidence: 99%

Origins of Type Ibn SNe 2006jc/2015G in interacting binaries and implications for pre-SN eruptions

Sun

Maund

Hirai

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…On the other hand, if it occurs earlier and is energetic enough it might help explain the outbursts (supernova impostors, SN IIn) that have been observed to occur in some supernova progenitors in the last years and decades before the explosion (Smith et al 2011;Smith & Arnett 2014;Ofek et al 2014;Arcavi et al 2017). The energy generated by a shell merger deep in the star's compact core might be transported to the envelope via waves as proposed by Quataert & Shiode (2012) and later investigated by Shiode & Quataert (2014), Fuller (2017, and Fuller & Ro (2018). Jones et al (2017, J17 hereafter) presented a set of idealised 3D hydrodynamic simulations constructed to closely resemble a convective O-burning shell in their 1D model of a 25 M star.…”

Section: Introductionmentioning

confidence: 98%

3D hydrodynamic simulations of C ingestion into a convective O shell

Andrássy

Herwig

Woodward

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Interactions between convective shells in evolved massive stars have been linked to supernova impostors, to the production of the odd-Z elements Cl, K, and Sc, and they might also help generate the large-scale asphericities that are known to facilitate shock revival in supernova explosion models. We investigate the process of ingestion of Cshell material into a convective O-burning shell, including the hydrodynamic feedback from the nuclear burning of the ingested material. Our 3D hydrodynamic simulations span almost 3 dex in the total luminosity L tot . All but one of the simulations reach a quasi-stationary state with the entrainment rate and convective velocity proportional to L tot and L 1/3 tot , respectively. Carbon burning provides 14 -33% of the total luminosity, depending on the set of reactions considered. Equivalent simulations done on 768 3 and 1152 3 grids are in excellent quantitative agreement. The flow is dominated by a few large-scale convective cells. An instability leading to large-scale oscillations with Mach numbers in excess of 0.2 develops in an experimental run with the energy yield from C burning increased by a factor of 10. This run represents most closely the conditions expected in a violent O-C shell merger, which is a potential production site for odd-Z elements such as K and Sc and which may seed asymmetries in the supernova progenitor. 1D simulations may underestimate the energy generation from the burning of ingested material by as much as a factor two owing to their missing the effect of clumpiness of entrained material on the nuclear reaction rate.

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“…On the other hand, for model YSG, central carbon burning is still continuing at 0.1 years before core collapse. classes, namely super-Eddington winds (Quataert et al 2016;Fuller & Ro 2018;Ouchi & Maeda 2019) and non-terminal explosions (Dessart et al 2010;Owocki et al 2019). These classes seem to correspond to continuous and instantaneous extra energy injection, respectively.…”

Section: Introductionmentioning

confidence: 99%

Radiation hydrodynamical simulations of eruptive mass loss from progenitors of Type Ibn/IIn supernovae

Kuriyama

Shigeyama

2020

A&A

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Context. Observations suggest that some massive stars experience violent and eruptive mass loss associated with significant brightening that can not be explained by hydrostatic stellar models. This event seemingly forms dense circumstellar matter (CSM). The mechanism of eruptive mass loss has not been clarified. We focus on the fact that the timescale of nuclear burning gets shorter than the dynamical timescale of the envelope a few years before core collapse for some massive stars. Aims. To reveal the properties of the eruptive mass loss, we investigate its relation to the energy injection at the bottom of the envelope supplied by nuclear burning taking place inside the core. In this study, we do not specify the actual mechanism to transport energy from the site of nuclear burning to the bottom of the envelope. Instead, we parameterize the amount of injected energy and the injection time and try to extract information on these parameters from comparisons with observations. Methods. To this end, we carried out 1-D radiation hydrodynamical simulations for progenitors of red, yellow, and blue supergiants, and Wolf-Rayet stars. We calculated the evolution of the progenitors with a public stellar evolution code. Results. We obtained the light curve associated with the eruption, the amount of ejected mass, and the CSM distribution at the time of core-collapse. Conclusions. The energy injection at the bottom of the envelope of a massive star within a period shorter than the dynamical timescale of the envelope could reproduce some observed optical outbursts prior to the core-collapse and form the CSM, which can power an interaction SN classified as type IIn.

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Pre-supernova outbursts via wave heating in massive stars – II. Hydrogen-poor stars

Cited by 125 publications

References 81 publications

Origins of Type Ibn SNe 2006jc/2015G in interacting binaries and implications for pre-SN eruptions

Origins of Type Ibn SNe 2006jc/2015G in interacting binaries and implications for pre-SN eruptions

3D hydrodynamic simulations of C ingestion into a convective O shell

Radiation hydrodynamical simulations of eruptive mass loss from progenitors of Type Ibn/IIn supernovae

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