Impact of common envelope development criteria on the formation of LIGO/Virgo sources

Olejak, Aleksandra; Belczyński, Krzysztof; Іванова, Наталя

doi:10.1051/0004-6361/202140520

Cited by 71 publications

(48 citation statements)

References 136 publications

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“…The prediction that the population of merging BBHs originates from a mixture of systems formed through the CE and stable RLOF channel, has been reported by various authors based on simulations with different codes and we thus believe this to be robust (e.g. van den Heuvel et al 2017;Bavera et al 2021;Marchant et al 2021;Broekgaarden et al 2021;Gallegos-Garcia et al 2021;Shao & Li 2021;Olejak et al 2021). Moreover, the bimodality in the delay time distribution has also been found in other work inspecting BBHs formed through the isolated binary formation channel; see e.g.…”

Section: Discussionsupporting

confidence: 81%

The redshift evolution of the binary black hole merger rate: a weighty matter

van Son,

de Mink,

Callister

et al. 2021

Preprint

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Gravitational wave detectors are starting to reveal the redshift evolution of the binary black hole (BBH) merger rate, R BBH (z). We make predictions for R BBH (z) as a function of black hole mass for systems originating from isolated binaries. To this end, we investigate correlations between the delay time and black hole mass by means of the suite of binary population synthesis simulations, COMPAS. We distinguish two channels: the common envelope (CE), and the stable Roche-lobe overflow (RLOF) channel, characterised by whether the system has experienced a common envelope or not. We find that the CE channel preferentially produces BHs with masses below about 30 M and short delay times (t delay 1 Gyr), while the stable RLOF channel primarily forms systems with BH masses above 30 M and long delay times (t delay 1 Gyr). We provide a new fit for the metallicity specific starformation rate density based on the Illustris TNG simulations, and use this to convert the delay time distributions into a prediction of R BBH (z). This leads to a distinct redshift evolution of R BBH (z) for high and low primary BH masses. We furthermore find that, at high redshift, R BBH (z) is dominated by the CE channel, while at low redshift it contains a large contribution (∼ 40%) from the stable RLOF channel. Our results predict that, for increasing redshifts, BBHs with component masses above 30 M will become increasingly scarce relative to less massive BBH systems. Evidence of this distinct evolution of R BBH (z) for different BH masses can be tested with future detectors.

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Section: Discussionsupporting

confidence: 81%

The redshift evolution of the binary black hole merger rate: a weighty matter

van Son,

de Mink,

Callister

et al. 2021

Preprint

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“…The situation is even more complex when considering that our larger suite of models (560 realizations) still only represents a subset of the overall uncertainties in population synthesis studies. For example, even our broader set of models does not account for uncertainties in the stellar evolution tracks (e.g., Laplace et al 2020;Agrawal et al 2020), internal mixing (e.g., Schootemeĳer et al 2019), stellar rotation (e.g., de Mink & Mandel 2016Mapelli et al 2020), the more complex physics of the CE phase (e.g., Klencki et al 2021;Ivanova et al 2020;Marchant et al 2021;Olejak et al 2021), the additional possible remnant mass prescriptions (e.g. Dabrowny et al 2021;, the initial conditions of binary systems (e.g., de Mink & Belczynski 2015;Moe & Di Stefano 2017;Klencki et al 2018), and the possible contributions from other formation channels (e.g., Zevin et al 2021).…”

Section: A Realistic View Of Population Synthesis Modelsmentioning

confidence: 99%

Impact of Massive Binary Star and Cosmic Evolution on Gravitational Wave Observations II: Double Compact Object Rates and Properties

Broekgaarden,

Berger,

Stevenson

et al. 2021

Preprint

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Making the most of the rapidly increasing population of gravitational-wave detections of black hole (BH) and neutron star (NS) mergers requires comparing observations with population synthesis predictions. In this work we investigate the combined impact from the key uncertainties in population synthesis modelling of the isolated binary evolution channel: the physical processes in massive binary-star evolution and the star formation history as a function of metallicity, 𝑍, and redshift 𝑧, S(𝑍, 𝑧). Considering these uncertainties we create 560 different publicly available model realizations and calculate the rate and distribution characteristics of detectable BHBH, BHNS, and NSNS mergers. We find that our stellar evolution and S(𝑍, 𝑧) variations can impact the predicted intrinsic and detectable merger rates by factors 10 2 -10 4 . We find that BHBH rates are dominantly impacted by S(𝑍, 𝑧) variations, NSNS rates by stellar evolution variations and BHNS rates by both. We then consider the combined impact from all uncertainties considered in this work on the detectable mass distribution shapes (chirp mass, individual masses and mass ratio). We find that the BHNS mass distributions are predominantly impacted by massive binary-star evolution changes. For BHBH and NSNS we find that both uncertainties are important. We also find that the shape of the delay time and birth metallicity distributions are typically dominated by the choice of S(𝑍, 𝑧) for BHBH, BHNS and NSNS. We identify several examples of robust features in the mass distributions predicted by all 560 models, such that we expect more than 95 percent of BHBH detections to contain a BH 8 M and have mass ratios 4. Our work demonstrates that it is essential to consider a wide range of allowed models to study double compact object merger rates and properties. Conversely, larger observed samples could allow us to decipher currently unconstrained stages of stellar and binary evolution.

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“…In the case that the embedded companion is a BH, then feedback produced by the BH can be deposited into the envelope of the host star, potentially unbinding it and producing novel electromagnetic transients (Moreno Méndez et al 2017a;López-Cámara et al 2020). If the envelope unbinds before the BH merges with the core of the host star, then this will alter the configuration of the binary remnant, which could hinder the viability of common envelopes as formation channels for LIGO/Virgo sources (e.g., Olejak et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Jet Formation in 3D GRMHD Simulations of Bondi-Hoyle-Lyttleton Accretion

Kaaz¹,

Murguia-Berthier²,

Chatterjee³

et al. 2022

Preprint

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A black hole (BH) travelling through a uniform, gaseous medium is described by Bondi-Hoyle-Lyttleton (BHL) accretion. If the medium is magnetized, then the black hole can produce relativistic outflows. We performed the first 3D, general-relativistic magnetohydrodynamics simulations of BHL accretion onto rapidly rotating black holes using the code H-AMR, where we mainly varied the strength of a background magnetic field that threads the medium. We found that the ensuing accretion continuously drags to the BH the magnetic flux, which accumulates near the event horizon until it becomes dynamically important. Depending on the strength of the background magnetic field, the BHs can sometimes launch relativistic jets with high enough power to drill out of the inner accretion flow, become bent by the headwind, and escape to large distances. While for stronger background magnetic fields the jets are continuously powered, at weaker field strengths they are intermittent, turning on and off depending on the fluctuating gas and magnetic flux distributions near the event horizon. We find that our jets reach extremely high efficiencies of ∼ 100 − 300%, even in the absence of an accretion disk. We also calculated the drag forces exerted by the gas onto to the BH, finding that the presence of magnetic fields causes drag forces to be much less efficient than in unmagnetized BHL accretion, and sometimes become negative, accelerating the BH rather than slowing it down. Our results extend classical BHL accretion to rotating BHs moving through magnetized media and demonstrate that accretion and drag are significantly altered in this environment.

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Impact of common envelope development criteria on the formation of LIGO/Virgo sources

Cited by 71 publications

References 136 publications

The redshift evolution of the binary black hole merger rate: a weighty matter

The redshift evolution of the binary black hole merger rate: a weighty matter

Impact of Massive Binary Star and Cosmic Evolution on Gravitational Wave Observations II: Double Compact Object Rates and Properties

Jet Formation in 3D GRMHD Simulations of Bondi-Hoyle-Lyttleton Accretion

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