The death of massive stars - II. Observational constraints on the progenitors of Type Ibc supernovae

Eldridge, J. J.; Fraser, M.; Smartt, S. J.; Maund, Justyn R.; Crockett, R. M.

doi:10.1093/mnras/stt1612

Cited by 293 publications

(385 citation statements)

References 172 publications

(215 reference statements)

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“…We synthesise magnitudes data for our models using the bpass code (for a complete description, see Eldridge & Stanway 2009;Eldridge et al 2013). In Figs.…”

Section: The Deaths Of Helium Starsmentioning

confidence: 99%

“…With our grids of helium star models, we provide an evolutionary test of this conclusion. Previous theoretical studies on the evolution of WR stars have considered the effects of rotation (Georgy et al 2012;Meynet & Maeder 2005) and duplicity (Vanbeveren et al 1998;Van Bever & Vanbeveren 2003;Vanbeveren, Van Bever & Belkus 2007;Eldridge et al 2013). Following Habets (1986) and Dewi et al (2002), we shall investigate the evolution of single helium star models.…”

Section: Introductionmentioning

confidence: 99%

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Helium stars: towards an understanding of Wolf–Rayet evolution

McClelland

Eldridge

2016

Mon. Not. R. Astron. Soc.

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Wolf-Rayet (WR) stars are massive stars that have lost most or all of their hydrogen via powerful stellar winds. Recent observations have indicated that hydrogen-free WR stars have cooler temperatures than those predicted by current evolutionary models. To investigate how varying mass-loss rate affects WR evolution, we have created a grid of pure helium star models. We compare our results with Galactic and LMC WR observations and show that the temperature ranges of observed WR stars can be reproduced by varying the mass-loss rate, which effectively determines the size of the helium envelope around the core. We also find that WN and WO stars arise from more massive stars, whereas WC stars come from lower masses. This contradicts the standard Conti scenario by which WN and WC stars evolve in an age sequence. We also predict the magnitudes of our models at core-collapse and compare with observations of nearby progenitors of Type Ib/c supernovae. We confirm the findings of previous studies that suggest WR stars are the progenitors of core-collapse supernovae: the progenitors would remain unobserved except in the cases where the progenitor is a low-mass helium giant, as is the case of iPTF13bvn.

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“…We synthesise magnitudes data for our models using the bpass code (for a complete description, see Eldridge & Stanway 2009;Eldridge et al 2013). In Figs.…”

Section: The Deaths Of Helium Starsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Helium stars: towards an understanding of Wolf–Rayet evolution

McClelland

Eldridge

2016

Mon. Not. R. Astron. Soc.

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“…If they can produce supernovae at their death, they would appear as Type Ib or Ic supernovae (SNe Ib/Ic). Hydrogen-deficient stars as SN Ib/Ic progenitors may also be produced in interacting binary systems, and they can be less massive than classical WR stars that typically have M > 10 M ⊙ (Podsiadlowski et al 1992;Vanbeveren et al 1998;Wellstein et al 1999;Yoon et al 2010;Eldridge et al 2013;Yoon et al 2017). The quasi-WR star HD45166 is one such candidate (e.g., Steiner & Oliveira 2005).…”

Section: Introductionmentioning

confidence: 99%

Towards a better understanding of the evolution of Wolf–Rayet stars and Type Ib/Ic supernova progenitors

Yoon

2017

Monthly Notices of the Royal Astronomical Society

114

160

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Hydrogen-deficient Wolf-Rayet (WR) stars are potential candidates of Type Ib/Ic supernova (SN Ib/Ic) progenitors and their evolution is governed by mass loss. Stellar evolution models with the most popular prescription for WR mass-loss rates given by Nugis & Lamers have difficulties in explaining the luminosity distribution of WR stars of WC and WO types and the SN Ic progenitor properties. Here we suggest some improvements in the WR mass-loss rate prescription and discuss its implications for the evolution of WR stars and SN Ib/Ic progenitors. Recent studies on Galactic WR stars clearly indicate that the mass-loss rates of WC stars are systematically higher than those of WNE stars for a given luminosity. The luminosity and initial metallicity dependencies of WNE mass-loss rates are also significantly different from those of WC stars. These factors have not been adequately considered together in previous stellar evolution models. We also find that an overall increase of WR mass loss rates by about 60 per cent compared to the empirical values obtained with a clumping factor of 10 is needed to explain the most faint WC/WO stars. This moderate increase with our new WR mas-loss rate prescription results in SN Ib/Ic progenitor models more consistent with observations than those given by the Nugis & Lamers prescription. In particular, our new models predict that the properties of SN Ib and SN Ic progenitors are distinctively different, rather than they form a continuous sequence.

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“…The less massive ZAMS mass stars need to remove their hydrogen-rich envelopes with mass loss caused by binary interactions because of their inefficient radiationdriven wind (e.g., Podsiadlowski, Joss, & Hsu 1992;Nomoto, Iwamoto, & Suzuki 1995;Podsiadlowski et al 2004b;Izzard, Ramirez-Ruiz, & Tout 2004;Yoon, Woosley, & Langer 2010;Eldridge, Langer, & Tout 2011;Benvenuto, Bersten, & Nomoto 2013;Lyman et al 2016a;Eldridge & Maund 2016). It is also known that mass loss caused by binary interaction is essential to explain the observational ratio of stripped-envelope SNe to hydrogen-rich SNe (e.g., Eldridge, Izzard, & Tout 2008;Eldridge et al 2013;Smith et al 2011).…”

Section: Introductionmentioning

confidence: 99%

Light-curve and spectral properties of ultrastripped core-collapse supernovae leading to binary neutron stars

Moriya

Mazzali

Tominaga

et al. 2016

Mon. Not. R. Astron. Soc.

105

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We investigate light-curve and spectral properties of ultra-stripped core-collapse supernovae. Ultra-stripped supernovae are the explosions of heavily stripped massive stars which lost their envelopes via binary interactions with a compact companion star. They eject only ∼ 0.1 M ⊙ and may be the main way to form double neutronstar systems which eventually merge emitting strong gravitational waves. We follow the evolution of an ultra-stripped supernova progenitor until iron core collapse and perform explosive nucleosynthesis calculations. We then synthesize light curves and spectra of ultra-stripped supernovae using the nucleosynthesis results and present their expected properties. Ultra-stripped supernovae synthesize ∼ 0.01 M ⊙ of radioactive 56 Ni, and their typical peak luminosity is around 10 42 erg s −1 or −16 mag. Their typical rise time is 5 − 10 days. Comparing synthesized and observed spectra, we find that SN 2005ek, some of the so-called calcium-rich gap transients, and SN 2010X may be related to ultra-stripped supernovae. If these supernovae are actually ultra-stripped supernovae, their event rate is expected to be about 1 per cent of core-collapse supernovae. Comparing the double neutron-star merger rate obtained by future gravitational-wave observations and the ultra-stripped supernova rate obtained by optical transient surveys identified with our synthesized light-curve and spectral models, we will be able to judge whether ultra-stripped supernovae are actually a major contributor to the binary neutron star population and provide constraints on binary stellar evolution.

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The death of massive stars - II. Observational constraints on the progenitors of Type Ibc supernovae

Cited by 293 publications

References 172 publications

Helium stars: towards an understanding of Wolf–Rayet evolution

Helium stars: towards an understanding of Wolf–Rayet evolution

Towards a better understanding of the evolution of Wolf–Rayet stars and Type Ib/Ic supernova progenitors

Light-curve and spectral properties of ultrastripped core-collapse supernovae leading to binary neutron stars

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