Explodability fluctuations of massive stellar cores enable asymmetric compact object mergers such as GW190814

Antoniadis, John; Aguilera-Dena, David R.; Vigna-Gómez, Alejandro; Krämer, M.; Langer, N.; Müller, Bernhard; Tauris, T. M.; Wang, C.; Xu, Xiao-Tian

doi:10.1051/0004-6361/202142322

Cited by 10 publications

(16 citation statements)

References 73 publications

(91 reference statements)

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“…If this is indeed the case, then the need arises to study this effect in more detail, to be able to better interpret the distributions of BH masses that will become available from future observations of binary BH mergers. The formation of such systems may help explain the asymmetric compact object mergers that have been recently detected by LIGO (Antoniadis et al 2022). A final trend that is noteworthy in the BH mass distribution is a change in the slope of the distribution of BHs above a certain mass, also found by Woosley et al (2020), caused by the change in the implemented mass loss rate from WN-type mass loss to WC-type mass loss; which corresponds to the change in trend in final mass shown in Fig.…”

Section: Compact Object Populationsmentioning

confidence: 98%

“…We discuss the impact of parameter variation, as well as the impact of the binding energy that is used to calculate the outcome of the explosions in Appendix B. The models from Set B, presented in Appendix B.2, correspond to those used by Antoniadis et al (2022).…”

Section: Explodability Criteria and Observable Supernova Propertiesmentioning

confidence: 99%

“…A.2). Because all of the explosions predicted in this regime are powered by fallback, we refer to this region as the "island of fallback explodability" (see Antoniadis et al 2022, for a discussion). The exact number of fallback SNe, as well as their properties, depend sensitively Circles represent models with final surface abundances that correspond to Type Ib SN progenitors, whereas crosses represent models with surface abundances that correspond to Type Ic SN progenitors.…”

Section: Properties Of Supernova Explosions From Stripped-envelope Starsmentioning

confidence: 99%

“…Zevin et al 2020), even when considering the possibility of explodability islands (Mandel et al 2021). This idea is explored further by Antoniadis et al (2022).…”

Section: Compact Object Formation and Islands Of Explodabilitymentioning

confidence: 99%

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Stripped-envelope stars in different metallicity environments

Aguilera-Dena

Langer

Antoniadis

et al. 2022

A&A

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Massive stars that become stripped of their hydrogen envelope through binary interaction or winds can be observed either as Wolf-Rayet stars, if they have optically thick winds, or as transparent-wind stripped-envelope stars. We approximate their evolution through evolutionary models of single helium stars, and compute detailed model grids in the initial mass range 1.5−70 M⊙ for metallicities between 0.01 and 0.04, from core helium ignition until core collapse. Throughout their lifetimes some stellar models expose the ash of helium burning. We propose that models that have nitrogen-rich envelopes are candidate WN stars, while models with a carbon-rich surface are candidate WC stars during core helium burning, and WO stars afterwards. We measure the metallicity dependence of the total lifetimes of our models and the duration of their evolutionary phases. We propose an analytic estimate of the wind’s optical depth to distinguish models of Wolf-Rayet stars from transparent-wind stripped-envelope stars, and find that the luminosity ranges at which WN-, WC-, and WO-type stars can exist is a strong function of metallicity. We find that all carbon-rich models produced in our grids have optically thick winds and match the luminosity distribution of observed populations. We construct population models and predict the numbers of transparent-wind stripped-envelope stars and Wolf-Rayet stars, and derive their number ratios at different metallicities. We find that as metallicity increases, the number of transparent-wind stripped-envelope stars decreases and the number of Wolf-Rayet stars increases. At high metallicities WC- and WO-type stars become more common. We apply our population models to nearby galaxies, and find that populations are more sensitive to the transition luminosity between Wolf-Rayet stars and transparent-wind helium stars than to the metallicity-dependent mass loss rates.

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Section: Compact Object Populationsmentioning

confidence: 98%

Section: Explodability Criteria and Observable Supernova Propertiesmentioning

confidence: 99%

Section: Properties Of Supernova Explosions From Stripped-envelope Starsmentioning

confidence: 99%

“…Zevin et al 2020), even when considering the possibility of explodability islands (Mandel et al 2021). This idea is explored further by Antoniadis et al (2022).…”

Section: Compact Object Formation and Islands Of Explodabilitymentioning

confidence: 99%

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Stripped-envelope stars in different metallicity environments

Aguilera-Dena

Langer

Antoniadis

et al. 2022

A&A

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“…We also choose to exclude the highly asymmetric binary GW190814 (Abbott et al 2020d), partly due to the uncertain classification of the secondary (which may either be the most massive neutron star or lightest black hole observed), and partly due to the mass ratio, which is difficult to produce though isolated binary evolution (though see Zevin et al 2020;Mandel et al 2020;Antoniadis et al 2022, for possible explanations in this context). We assume that the remainder of the population (79 events) are binary black holes.…”

Section: Observational Samplementioning

confidence: 99%

Constraints on the contributions to the observed binary black hole population from individual evolutionary pathways in isolated binary evolution

Stevenson

Clarke

2022

Monthly Notices of the Royal Astronomical Society

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Gravitational waves from merging binary black holes can be used to shed light on poorly understood aspects of massive binary stellar evolution, such as the evolution of massive stars (including their mass-loss rates), the common envelope phase, and the rate at which massive stars form throughout the cosmic history of the Universe. In this paper we explore the correlated impact of these phases on predictions for the merger rate and chirp mass distribution of merging binary black holes, aiming to identify possible degeneracies between model parameters. In many of our models, a large fraction (more than 70 per cent of detectable binary black holes) arise from the chemically homogeneous evolution scenario; these models tend to over-predict the binary black hole merger rate and produce systems which are on average too massive. Our preferred models favour enhanced mass-loss rates for helium rich Wolf–Rayet stars, in tension with recent theoretical and observational developments. We identify correlations between the impact of the mass-loss rates of Wolf–Rayet stars and the metallicity evolution of the Universe on the rates and properties of merging binary black holes. Based on the observed mass distribution, we argue that the $\sim 10{{\%}}$ of binary black holes with chirp masses greater than 40 M⊙ (the maximum predicted by our models) are unlikely to have formed through isolated binary evolution, implying a significant contribution (>10 per cent) from other formation channels such as dense star clusters or active galactic nuclei. Our models will enable inference on the uncertain parameters governing binary evolution in the near future.

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Thermonuclear and electron-capture supernovae from stripped-envelope stars

Chanlaridis

Antoniadis

Aguilera-Dena

et al. 2022

A&A

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Context. When stripped from their hydrogen-rich envelopes, stars with initial masses between ∼7 and 11 M ⊙ may 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 recently been 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 Iaand this 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 precollapse 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 modeled the evolution of 252 single, nonrotating helium stars covering the initial mass range 0.8-3.5 M ⊙ , with 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 used these models to constrain several properties of these stars, including their central densities, compositions, envelope masses, and radii at the onset explosive oxygen ignition, as well as 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 constrained 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 degenerate cores that retain more than approximately 0.005 M ⊙ of carbon result in (C)ONe SNe Ia, while those with lower carbon mass become ECSNe. We find that (C)ONe SNe Ia are more likely to occur at high metallicities, whereas at low metallicities ECSNe dominate. However, both SN Ia and ECSN progenitors expand significantly during the final evolutionary stages, so that for the most extended models, a further binary interaction may occur. 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 ...

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Explodability fluctuations of massive stellar cores enable asymmetric compact object mergers such as GW190814

Cited by 10 publications

References 73 publications

Stripped-envelope stars in different metallicity environments

Stripped-envelope stars in different metallicity environments

Constraints on the contributions to the observed binary black hole population from individual evolutionary pathways in isolated binary evolution

Thermonuclear and electron-capture supernovae from stripped-envelope stars

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