Mass-Loss Rates of Very Massive Stars

Vink, Jorick S.

doi:10.1007/978-3-319-09596-7_4

Cited by 27 publications

(11 citation statements)

References 92 publications

(109 reference statements)

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“…We note that the estimated mass-loss rate of SN 2008es is very high compared to known massive stellar winds, at most 10 −3 M ⊙ yr −1 with v w ≈ 10 km s −1 for extreme red supergiants (RSGs) (Smith 2014;Vink 2015;. The mechanism for this extreme mass loss a few years before the explosion is still unknown, but is believed to be either by binary interaction ( 10 −1 M ⊙ yr −1 with v w ≈ 10-100 km s −1 ) or a luminous blue variable (LBV)-like giant eruption ( 10 M ⊙ yr −1 with v w ≈ 100-1000 km s −1 ) such as those observed in η Carinae or P Cygni (Smith et al 2003;Smith & Hartigan 2006;Smith & Owocki 2006;Smith 2014Chevalier 2012).…”

Section: Csimentioning

confidence: 89%

The Type II superluminous SN 2008es at late times: near-infrared excess and circumstellar interaction

Bhirombhakdi

Chornock

Miller

et al. 2019

Monthly Notices of the Royal Astronomical Society

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SN 2008es is one of the rare cases of a Type II superluminous supernova (SLSN) showing no relatively narrow features in its early-time spectra, and therefore its powering mechanism is under debate between circumstellar interaction (CSI) and magnetar spin-down. Late-time data are required for better constraints. We present optical and near-infrared (NIR) photometry obtained from Gemini, Keck, and Palomar Observatories from 192 to 554 days after explosion. Only broad Hα emission is detected in a Gemini spectrum at 288 days. The line profile exhibits red-wing attenuation relative to the early-time spectrum. In addition to the cooling SN photosphere, a NIR excess with blackbody temperature ∼ 1500 K and radius ∼ 10 16 cm is observed. This evidence supports dust condensation in the cool dense shell being responsible for the spectral evolution and NIR excess. We favour CSI, with ∼ 2-3 M ⊙ of circumstellar material (CSM) and ∼10-20 M ⊙ of ejecta, as the powering mechanism, which still dominates at our late-time epochs. Both models of uniform density and steady wind fit the data equally well, with an effective CSM radius ∼ 10 15 cm, supporting the efficient conversion of shock energy to radiation by CSI. A low amount ( 0.4 M ⊙ ) of 56 Ni is possible but cannot be verified yet, since the light curve is dominated by CSI. The magnetar spin-down powering mechanism cannot be ruled out, but is less favoured because it overpredicts the late-time fluxes and may be inconsistent with the presence of dust.

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Section: Csimentioning

confidence: 89%

The Type II superluminous SN 2008es at late times: near-infrared excess and circumstellar interaction

Bhirombhakdi

Chornock

Miller

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…The most promising scenario for eruptive mass loss has been proposed by Owocki et al (2004), who developed a theory of 'porosity-moderated mass loss' (see also Shaviv 1998Shaviv , 2000. As LBVs find themselves in close proximity to the Eddington limit, we can be confident that radiation pressure will play a role in the driving of an outflow (Owocki 2015;Vink 2015). This is even more likely now that empirical mass-loss rates in close proximity to the Eddington limit have been found to increase steeply (Bestenlehner et al 2014) -in agreement with theoretical expectations of Gräfener et al (2011);Vink et al (2011); Vink & Gräfener (2012).…”

Section: Introductionmentioning

confidence: 99%

Two bi-stability jumps in theoretical wind models for massive stars and the implications for luminous blue variable supernovae

Petrov¹,

Gräfener²

2016

Mon. Not. R. Astron. Soc.

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Luminous Blue Variables have been suggested to be the direct progenitors of supernova types IIb and IIn, with enhanced mass loss prior to explosion. However, the mechanism of this mass loss is not yet known. Here, we investigate the qualitative behaviour of theoretical stellar wind mass-loss as a function of T eff across two bi-stability jumps in blue supergiant regime and also in proximity to the Eddington limit, relevant for LBVs. To investigate the physical ingredients that play a role in the radiative acceleration we calculate blue supergiant wind models with the cmfgen non-LTE model atmosphere code over an effective temperature range between 30 000 and 8 800 K. Although our aim is not to provide new mass-loss rates for BA supergiants, we study and confirm the existence of two bi-stability jumps in mass-loss rates predicted by Vink, de Koter, & Lamers (1999). However, they are found to occur at somewhat lower T eff (20 000 and 9 000 K, respectively) than found previously, which would imply that stars may evolve towards lower T eff before strong mass-loss is induced by the bistability jumps. When the combined effects of the second bi-stability jump and the proximity to Eddington limit are accounted for, we find a dramatic increase in the mass-loss rate by up to a factor of 30. Further investigation of both bi-stability jumps is expected to lead to a better understanding of discrepancies between empirical modelling and theoretical mass-loss rates reported in the literature, and to provide key inputs for the evolution of both normal AB supergiants and LBVs, as well as their subsequent supernova type II explosions.

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“…The amount of radioactive nickel generated during the explosion phase may be as high as 55 M⊙ resulting in a very bright supernova event. Nevertheless, the major uncertainties in the evolution of very massive stars are the mass-loss prescriptions and the treatment of convection (Vink 2015;Woosley & Heger 2015).…”

Section: Introductionmentioning

confidence: 99%

“…Recent studies clearly show that metal-free (Z = 0) or almost metal-free (Z = 10 −4 Z⊙) PISN models retain a very massive hydrogen-rich envelope because of an absence of mass-loss or a very low mass-loss rate (Kasen et al 2011;Dessart et al 2013). There is a large uncertainty because mass-loss rates at low metallicity are extrapolated from rates derived for considerably higher metallicity (Hirschi 2007;Vink 2015). These metal-free progenitors originate in a low-metallicity environment, i.e.…”

Section: Introductionmentioning

confidence: 99%

Fast evolving pair-instability supernova models: evolution, explosion, light curves

Kozyreva

Gilmer

Hirschi

et al. 2016

Mon. Not. R. Astron. Soc.

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With an increasing number of superluminous supernovae (SLSNe) discovered the question of their origin remains open and causes heated debates in the supernova community. Currently, there are three proposed mechanisms for SLSNe: (1) pair-instability supernovae (PISN), (2) magnetar-driven supernovae, and (3) models in which the supernova ejecta interacts with a circumstellar material ejected before the explosion. Based on current observations of SLSNe, the PISN origin has been disfavoured for a number of reasons. Many PISN models provide overly broad light curves and too reddened spectra, because of massive ejecta and a high amount of nickel. In the current study we re-examine PISN properties using progenitor models computed with the GENEC code. We calculate supernova explosions with FLASH and light curve evolution with the radiation hydrodynamics code STELLA. We find that high-mass models (200 M⊙ and 250 M⊙) at relatively high metallicity (Z = 0.001) do not retain hydrogen in the outer layers and produce relatively fast evolving PISNe Type I and might be suitable to explain some SLSNe. We also investigate uncertainties in light curve modelling due to codes, opacities, the nickel-bubble effect and progenitor structure and composition.

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Mass-Loss Rates of Very Massive Stars

Cited by 27 publications

References 92 publications

The Type II superluminous SN 2008es at late times: near-infrared excess and circumstellar interaction

The Type II superluminous SN 2008es at late times: near-infrared excess and circumstellar interaction

Two bi-stability jumps in theoretical wind models for massive stars and the implications for luminous blue variable supernovae

Fast evolving pair-instability supernova models: evolution, explosion, light curves

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