Binary-Stripped Stars as Core-Collapse Supernovae Progenitors

Vartanyan, David; Laplace, Eva; Renzo, Mathieu; Götberg, Ylva; Burrows, Adam; de Mink, Selma E.

doi:10.48550/arxiv.2104.03317

Cited by 6 publications

(7 citation statements)

References 71 publications

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“…This is due to the extra mass loss binaries undergo, lowering the final helium core masses. Thus for a given helium core mass at core-collapse binary-stripped systems have a higher initial mass (Kippenhahn & Weigert 1967;Habets 1986), expanding the range in initial masses over which we assume a successful explosion occurs (Vartanyan et al 2021). For our systems, a cut of M He,final < 7 M is equivalent to a cut of M init < 19 M for single stars and M init < 22 M for binaries.…”

Section: Bh Formation Assumptionmentioning

confidence: 85%

The cosmic carbon footprint of massive stars stripped in binary systems

Farmer,

Laplace,

de Mink

et al. 2021

Preprint

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The cosmic origin of carbon, a fundamental building block of life, is still uncertain. Yield predictions for massive stars are almost exclusively based on single star models, even though a large fraction interact with a binary companion. Using the MESA stellar evolution code, we predict the carbon ejected in the winds and supernovae of single and binary-stripped stars at solar metallicity. We find that binary-stripped stars are twice as efficient at producing carbon (1.5-2.6 times, depending on choices on the slope of the initial mass function and black hole formation). We confirm that this is because the convective helium core recedes in stars that have lost their hydrogen envelope, as noted previously. The shrinking of the core disconnects the outermost carbon-rich layers created during the early phase of helium burning from the more central burning regions. The same effect prevents carbon destruction, even when the supernova shock wave passes. The yields are sensitive to the treatment of mixing at convective boundaries, specifically during carbon-shell burning (variations up to 40%) and improving upon this should be a central priority for more reliable yield predictions. The yields are robust (variations less than 0.5%) across our range of explosion assumptions. Black hole formation assumptions are also important, implying that the stellar graveyard now explored by gravitationalwave detections may yield clues to better understand the cosmic carbon production. Our findings also highlight the importance of accounting for binary-stripped stars in chemical yield predictions and motivates further studies of other products of binary interactions.

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Section: Bh Formation Assumptionmentioning

confidence: 85%

The cosmic carbon footprint of massive stars stripped in binary systems

Farmer,

Laplace,

de Mink

et al. 2021

Preprint

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show abstract

“…Previous studies have shown that the suggested explodability metrics depend on metallicity and rotation (O'Connor & Ott 2011), the adopted stellar wind mass-loss rates (even if these only act early during a star's evolution, Renzo et al 2017), overshooting (Davis et al 2019), and occurrence of convective shell mergers (e.g., Vartanyan et al 2021). Other parameters might play a significant role in shaping the density structure of the core at the onset of core collapse.…”

Section: Conclusion and Discussionmentioning

confidence: 98%

Revisiting the explodability of single massive star progenitors of stripped-envelope supernovae

Zapartas,

Renzo,

Fragos

et al. 2021

Preprint

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Stripped-envelope supernovae (Type IIb, Ib, Ic) showing little or no hydrogen are one of the main classes of explosions of massive stars. Their origin and the evolution of their progenitors are not fully understood as yet. Very massive single stars stripped by their own winds ( 25 − 30M at solar metallicity) are considered viable progenitors of these events. However, recent 1D core-collapse simulations show that some massive stars may collapse directly onto black holes after a failed explosion, with weak or no visible transient. In this letter, we estimate the effect of direct collapse onto a black hole on the rates of stripped-envelope supernovae that arise from single stars. For this, we compute single star MESA models at solar metallicity and map their final state to their corecollapse outcome following prescriptions commonly used in population synthesis. According to our models, no single stars that have lost their entire hydrogen-rich envelope are able to explode, and only a fraction of progenitors with a thin hydrogen envelope left (IIb progenitor candidates) do, unless we invoke increased wind mass-loss rates. This result increases the existing tension between the single-star scenario for stripped-envelope supernovae and their observed rates and properties. At face value, our results point towards an even higher contribution of binary progenitors for stripped-envelope supernovae. Alternatively, they may suggest inconsistencies in the common practice of mapping different stellar models to core-collapse outcomes and/or higher overall mass loss in massive stars.

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“…This is unfeasible for now as the computational expense is quite large. Recent studies of the single and binary progenitors of core-collapse supernovae evolved all the way to core-collapse explore tens to hundreds of stars (e.g., Sukhbold et al 2016;Vartanyan et al 2021). Doing this for millions of stars is unrealistic.…”

Section: Discussionmentioning

confidence: 99%

Comparing Compact Object Distributions from Mass- and Presupernova Core Structure-based Prescriptions

Patton,

Sukhbold,

Eldridge

2021

Preprint

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Binary population synthesis (BPS) employs prescriptions to predict final fates, explosion or implosion, and remnant masses based on one or two stellar parameters at the evolutionary cutoff imposed by the code, usually at or near central carbon ignition. In doing this, BPS disregards the integral role late-stage evolution plays in determining the final fate, remnant type, and remnant mass within the neutrino-driven explosion paradigm. To highlight differences between a popular prescription which relies only on the core and final stellar mass and emerging methods which rely on a star's presupernova core structure, we generate a series of compact object distributions using three different methods for a sample population of single and binary stars computed in BPASS. The first method estimates remnant mass based on a star's carbon-oxygen (CO) core mass and final total mass. The second method uses the presupernova core structure based on the bare CO-core models of Patton & Sukhbold (2020) combined with a parameterized explosion criterion to first determine final fate and remnant type, then remnant mass. The third method associates presupernova helium-core masses with remnant masses determined from public explosion models which rely implicitly on core structure. We find that the core-/final mass-based prescription favors lower mass remnants, including a large population of mass gap black holes, and predicts neutron star masses which span a wide range, whereas the structure-based prescriptions favor slightly higher mass remnants, mass gap black holes only as low as 3.5 M , and predict neutron star mass distributions which cluster in a narrow range.

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Binary-Stripped Stars as Core-Collapse Supernovae Progenitors

Cited by 6 publications

References 71 publications

The cosmic carbon footprint of massive stars stripped in binary systems

The cosmic carbon footprint of massive stars stripped in binary systems

Revisiting the explodability of single massive star progenitors of stripped-envelope supernovae

Comparing Compact Object Distributions from Mass- and Presupernova Core Structure-based Prescriptions

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