The Tarantula Massive Binary Monitoring

Context. The recent gravitational wave measurements have demonstrated the existence of stellar mass black hole binaries. It is essential for our understanding of massive star evolution to identify the contribution of binary evolution to the formation of double black holes. Aims. A promising way to progress is investigating the progenitors of double black hole systems and comparing predictions with local massive star samples such as the population in 30 Doradus in the Large Magellanic Cloud (LMC). Methods. To this purpose, we analyse a large grid of detailed binary evolution models at LMC metallicity with initial primary masses between 10 and 40 M , and identify which model systems potentially evolve into a binary consisting of a black hole and a massive main sequence star. We then derive the observable properties of such systems, as well as peculiarities of the OB star component. Results. We find that ∼3% of the LMC late O and early B stars in binaries are expected to possess a black hole companion, when assuming stars with a final helium core mass above 6.6 M to form black holes. While the vast majority of them may be X-ray quiet, our models suggest that these may be identified in spectroscopic binaries, either by large amplitude radial velocity variations ( ∼ > 50 km s −1 ) and simultaneous nitrogen surface enrichment, or through a moderate radial velocity ( ∼ > 10 km s −1 ) and simultaneously rapid rotation of the OB star. The predicted mass ratios are such that main sequence companions could be excluded in most cases. A comparison to the observed OB+WR binaries in the LMC, Be/X-ray binaries, and known massive BH binaries supports our conclusion. Conclusions. We expect spectroscopic observations to be able to test key assumptions in our models, with important implications for massive star evolution in general, and for the formation of double-black hole mergers in particular.

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“…6). Existing surveys include the TMBM survey in the LMC (Almeida et al, 2017), and the Galactic LAMOST survey (Yi et al 2019).…”

Section: Ob+bh Binary Detection Strategiesmentioning

confidence: 99%

Properties of OB star−black hole systems derived from detailed binary evolution models

Langer

Schürmann

Stoll

et al. 2020

A&A

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“…Most massive stars are found in binary systems (e.g., Mason et al 2009;Sana & Evans 2011;Sana et al 2012;Kiminki & Kobulnicky 2012;Chini et al 2012;Kobulnicky et al 2014;Almeida et al 2017), where mass loss also determines the angular momentum losses, thus the orbital evolution, and ultimately the binary evolution path and its end point (merger, disruption of the binary system, double compact object binary, etc. ).…”

Section: Introductionmentioning

confidence: 99%

Systematic survey of the effects of wind mass loss algorithms on the evolution of single massive stars

Renzo¹,

Ott²,

Shore³

et al. 2017

A&A

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136

150

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Mass loss processes are a key uncertainty in the evolution of massive stars. They determine the amount of mass and angular momentum retained by the star, thus influencing its evolution and presupernova structure. Because of the high complexity of the physical processes driving mass loss, stellar evolution calculations must employ parametric algorithms, and usually only include wind mass loss. We carried out an extensive parameter study of wind mass loss and its effects on massive star evolution using the open-source stellar evolution code MESA. We provide a systematic comparison of wind mass loss algorithms for solar-metallicity, nonrotating, single stars in the initial mass range of 15 M to 35 M . We consider combinations drawn from two hot phase (i.e., roughly the main sequence) algorithms, three cool phase (i.e., post-main-sequence) algorithms, and two Wolf-Rayet mass loss algorithms. We discuss separately the effects of mass loss in each of these phases. In addition, we consider linear wind efficiency scale factors of 1, 0.33, and 0.1 to account for suggested reductions in mass loss rates due to wind inhomogeneities. We find that the initial to final mass mapping for each zero-age main-sequence (ZAMS) mass has a ∼50% uncertainty if all algorithm combinations and wind efficiencies are considered. The ad-hoc efficiency scale factor dominates this uncertainty. While the final total mass and internal structure of our models vary tremendously with mass loss treatment, final luminosity and effective temperature are much less sensitive for stars with ZAMS mass 30 M . This indicates that uncertainty in wind mass loss does not negatively affect estimates of the ZAMS mass of most single-star supernova progenitors from pre-explosion observations. Our results furthermore show that the internal structure of presupernova stars is sensitive to variations in both main sequence and post main-sequence mass loss. The compactness parameter ξ ∝ M/R(M) has been identified as a proxy for the "explodability" of a given presupernova model. We find that ξ varies by as much as 30% for models of the same ZAMS mass evolved with different wind efficiencies and mass loss algorithm combinations. This suggests that the details of the mass loss treatment might bias the outcome of detailed core-collapse supernova calculations and the predictions for neutron star and black hole formation.

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“…ECSN thus form the transition between massive oxygen-neon (ONe) white dwarfs (WD) and supernovae. As the majority of massive stars are observed to be part of a binary system which could impact its evolution (Kobulnicky & Fryer 2007;Sana et al 2012Sana et al , 2013Duchêne & Kraus 2013;Kobulnicky et al 2014;Almeida et al 2017), not only the observational properties of these stars will be very different from single stars , their final properties could also affect our understanding of the formation and evolution of NS+NS mergers which could be observed by the aLIGO/VIRGO network (Abbott et al 2016;Côté et al 2017).…”

Section: Introductionmentioning

confidence: 99%

Electron Capture Supernovae from Close Binary Systems

Poelarends

Wurtz

Tarka

et al. 2017

ApJ

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We present the first detailed study of the Electron Capture Supernova Channel (ECSN Channel) for a primary star in a close binary star system. Progenitors of ECSN occupy the lower end of the mass spectrum of supernovae progenitors and are thought to form the transition between white dwarfs progenitors and core collapse progenitors . The mass range for ECSN from close binary systems is thought to be wider than the range for single stars, because of the effects of mass transfer on the helium core. Using the MESA stellar evolution code we explored the parameter space of initial primary masses between 8 M and 17 M , using a large grid of models . We find that the initial primary mass and the mass transfer evolution are important factors in the final fate of stars in this mass range. Mass transfer due to Roche Lobe overflow during and after carbon burning causes the core to cool down so that it avoids neon ignition, even in helium-free cores with masses up to 1.52 M , which in single stars would ignite neon. If the core is able to contract to high enough densities for electron captures to commence, we find that, for the adopted Ledoux convection criterion, the initial mass range for the primary to evolve into an ECSN is between 13.5 M and 17.6 M . The mass ratio, initial period, and mass loss efficiency only marginally affect the predicted ranges.

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The Tarantula Massive Binary Monitoring

Cited by 135 publications

References 44 publications

Properties of OB star−black hole systems derived from detailed binary evolution models

Properties of OB star−black hole systems derived from detailed binary evolution models

Systematic survey of the effects of wind mass loss algorithms on the evolution of single massive stars

Electron Capture Supernovae from Close Binary Systems

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