Stripped-Envelope Stars in Different Metallicity Environments I. Evolutionary Phases, Classification and Populations

Aguilera-Dena, David R.; Langer, Norbert; Antoniadis, John; Pauli, Daniel; Dessart, Luc; Vigna-Gómez, Alejandro; Gräfener, Götz; Yoon, Sung-Chul

doi:10.48550/arxiv.2112.06948

Cited by 4 publications

(4 citation statements)

References 97 publications

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“…The helium burning lifetime of helium-star models in the metallicity range covered by our grids is largely insensitive to variations of this parameter. This is in contrast to what has been found for largermass helium-stars (M He,i 4 M ) which are subject to stronger mass-loss rates during core helium burning (Aguilera-Dena et al 2021). The influence of overshooting and initial composition is further discussed in Section 4.…”

Section: The Series I Grid -An Overviewmentioning

confidence: 75%

Thermonuclear and Electron-Capture Supernovae from Stripped-Envelope Stars

Chanlaridis¹,

Antoniadis²,

Aguilera-Dena³

et al. 2022

Preprint

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Context. When stripped from their hydrogen-rich envelopes, stars with initial masses between ∼7 and 11 M develop massive degenerate cores and collapse. Depending on the final structure and composition, the outcome can range from a thermonuclear explosion, to the formation of a neutron star in an electron-capture supernova (ECSN). It has been recently demonstrated that stars in this mass range may be more prone to disruption than previously thought: they may initiate explosive oxygen burning when their central densities are still below ρ c 10 9.6 g cm −3 . At the same time, their envelopes expand significantly, leading to the complete depletion of helium. This combination makes them interesting candidates for Type Ia Supernovae-which we call (C)ONe SNe Ia-and might have broader implications for the formation of neutron stars via ECSNe. Aims. To constrain the observational counterparts of (C)ONe SNe Ia and the key properties that enable them, it is crucial to constrain the evolution, composition, and pre-collapse structure of their progenitors, as well as the evolution of these quantities with cosmic time. In turn, this requires a detailed investigation of the final evolutionary stages preceding the collapse, and their sensitivity to input physics.Methods. Here, we model the evolution of 252 single, non-rotating helium-stars covering the initial mass range 0.8-3.5 M , metallicities between Z = 10 −4 and 0.02, and overshoot efficiency factors from f OV = 0.0 to 0.016 across all convective boundaries. We use these models to constrain several properties of these stars, including their central densities, compositions and envelope masses at the time of explosive oxygen ignition, and the final outcome as a function of initial helium-star mass. We further investigate the sensitivity of these properties to mass-loss rate assumptions using an additional grid of 110 models with varying wind efficiencies. Results. We find that helium-star models with masses between ∼1.8 and 2.7 M are able to evolve onto 1.35-1.37 M (C)ONe cores that initiate explosive burning at central densities between log 10 (ρ c /g cm −3 ) ∼ 9.3 and 9.6. We constrain the amount of residual carbon retained after core carbon burning as a function of initial conditions, and conclude that it plays a critical role in determining the final outcome: Chandrasekhar-mass cores with residual carbon mass fractions of X min ( 12 C) 0.004 result in (C)ONe SNe Ia, while those with lower carbon mass fractions become ECSNe. We find that (C)ONe SNe Ia are more likely to occur at high metallicities, whereas at low metallicities ECSNe dominate. We constrain the relative ratio between (C)ONe SNe Ia and SNe Ib/c to be 0.17-0.30 at Z = 0.02, and 0.03-0.13 at Z ≤ 10 −3 . Conclusions. We conclude with a discussion on potential observational properties of (C)ONe SNe Ia and their progenitors. In the few thousand years leading to the explosion, at least some progenitors should be identifiable as luminous metal-rich supergiants, embedded in hydrogen-free circumstellar nebulae.

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Section: The Series I Grid -An Overviewmentioning

confidence: 75%

Thermonuclear and Electron-Capture Supernovae from Stripped-Envelope Stars

Chanlaridis¹,

Antoniadis²,

Aguilera-Dena³

et al. 2022

Preprint

Self Cite

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“…In addition, all primary stars were assumed to have solar metallicity (Z=0.02). Changes in the metallicity of the supergiant may have an effect on the envelope's binding energy and consequent CE outcomes (Aguilera-Dena et al 2021;Klencki et al 2021).…”

Section: Comparing Low-mass and High-mass Resultsmentioning

confidence: 99%

Convection Reconciles the Difference in Efficiencies Between Low-Mass and High-Mass Common Envelopes

Wilson,

Nordhaus

2022

Preprint

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The formation pathways for gravitational-wave merger sources are predicted to include common envelope (CE) evolution. Observations of high-mass post-common envelope binaries suggest that energy transfer to the envelope during the CE phase must be highly efficient. In contrast, observations of low-mass post-CE binaries indicate energy transfer during the CE phase must be highly inefficient. Convection, a process present in low-mass and high-mass stars, naturally explains this dichotomy. Using observations of Wolf-Rayet binaries, we study the effects of convection and radiative losses on the predicted final separations of high-mass common envelopes. Despite robust convection in massive stars, the effect is minimal as the orbit decays well before convection can transport the liberated orbital energy to the surface. In low-mass systems, convective transport occurs faster then the orbit decays, allowing the system to radiatively cool thereby lowering the efficiency. The inclusion of convection reproduces observations of low-mass and high-mass binaries and remains a necessary ingredient for determining outcomes of common envelopes.

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“…If the helium star mass is higher than a certain limit (e.g., about 8M for solar metallicity; see Shenar et al 2020;Aguilera-Dena et al 2021 for recent related discussions), the mass-loss rate would be high enough for the helium star to appear as a WR star that is characterized by strong emission lines from an optically thick wind. The WR mass-loss rate has been inferred by many observational studies on WR stars in the local Universe.…”

Section: Evolution Of Massive Stars Towards Sne Ib/icmentioning

confidence: 99%

Effects of wind mass-loss on the observational properties of Type Ib and Ic supernova progenitors

Yoon¹,

Jung²,

Jin

et al. 2020

Proc. IAU

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Progenitors of Type Ib and Ic supernovae (SNe) are stripped envelope stars and provide important clues on the mass-loss history of massive stars. Direct observations of the progenitors before the supernova explosion would provide strong constraints on the exact nature of SN Ib/Ic progenitors. Given that stripped envelope massive stars can have an optically thick wind as in the case of Wolf-Rayet stars, the influence of the wind on the observational properties needs to be properly considered to correctly infer progenitor properties from pre-SN observations. Non-LTE stellar atmosphere models indicate that the optical brightness could be greatly enhanced with an optically thick wind because of lifting-up of the photosphere from the stellar surface to the wind matter, and line and free-free emissions. So far, only a limited number of SN Ib/Ic progenitor candidates have been reported, including iPTF13bvn, SN 2017ein and SN 2019yvr. We argue that these three candidates are a biased sample, being unusually bright in the optical compared to what is expected from typical SN Ib/Ic progenitors, and that mass-loss enhancement during the final evolutionary stage can explain their optical properties.

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Stripped-Envelope Stars in Different Metallicity Environments I. Evolutionary Phases, Classification and Populations

Cited by 4 publications

References 97 publications

Thermonuclear and Electron-Capture Supernovae from Stripped-Envelope Stars

Thermonuclear and Electron-Capture Supernovae from Stripped-Envelope Stars

Convection Reconciles the Difference in Efficiencies Between Low-Mass and High-Mass Common Envelopes

Effects of wind mass-loss on the observational properties of Type Ib and Ic supernova progenitors

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