The Uncertain Future of Massive Binaries Obscures the Origin of LIGO/Virgo Sources

Belczyński, Krzysztof; Romagnolo, A; Olejak, Aleksandra; Klencki, J.; Chattopadhyay, Debatri; Stevenson, S. P.; Miller, M. Coleman; Lasota, Jarosław; Crowther, P. A.

doi:10.3847/1538-4357/ac375a

Cited by 52 publications

(36 citation statements)

References 127 publications

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“…Besides the stellar collapse and SN engine mechanism which is the main subject of this work, there are many other uncertain processes that dictate the formation of DCO mergers. Some examples of such processes or parameters which may significantly influence physical properties of DCO mergers are: the metallicity-specific star formation rate density and initial mass function (Chruślińska et al 2020;Santoliquido et al 2021;Broekgaarden et al 2021a;Briel et al 2021;Kroupa & Jerabkova 2021), stellar winds (Vink et al 2001;Sander et al 2022), convection and overshooting (Klencki et al 2021;Belczynski et al 2022), NS and BH natal kicks (Mandel et al 2021;Igoshev et al 2021), type and rate of mass transfer and the outcome of stable/unstable RLOF (Vinciguerra et al 2020;Howitt et al 2020;Bavera et al 2020;Vigna-Gómez et al 2022). The assumptions adopted for this work are described in Section 2.…”

Section: Discussion Of Caveats and Uncertaintiesmentioning

confidence: 99%

The role of supernova convection for the lower mass gap in the isolated binary formation of gravitational wave sources

Olejak¹,

Fryer²,

Belczyński³

et al. 2022

Preprint

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Understanding astrophysical phenomena involving compact objects requires an insight about the engine behind core-collapse supernovae (SNe) and the fate of the stellar collapse of massive stars. In particular, this insight is crucial in developing an understanding of the origin and formation channels of the growing population of black hole-black hole (BH-BH), black holeneutron star (BH-NS) and neutron star-neutron star (NS-NS) mergers reported by The LIGO-Virgo-KAGRA Collaboration. To gain this understanding, we must tie our current knowledge of pre-SN stars properties and their potential explosions to the final NS or BH mass distribution. The timescale of convection growth may have a large effect on the strength of SN explosion and therefore also on the mass distribution of stellar remnants. In this study we adopt the new formulas for the relation between the pre-SN properties of the stars and their remnants from Fryer et al. 2022 in prep. into StarTrack population synthesis code and check how they impact population of double compact object (DCO) mergers formed via isolated binary evolution. The new formulas give one ability to test a wide spectrum of assumptions on the convection growth time. In particular, different variants of the formulas allow for a smooth transition between having a deep lower mass gap and a remnant mass distribution filled by massive NSs and low mass BHs. Because the nature of convection can affect the DCO mergers mass distribution, observations of these distributions can, in turn, be used to better understand the convection growth timescale in stars and their SNe explosions. In this paper we present distribution of masses, mass ratios and the local merger rate densities of DCO mergers for different variants of new remnant mass formulas. We test them together with different approaches to other highly uncertain processes: limit for pair-instability SN and RLOF stability criteria. We find that mass distribution of DCO mergers (mass of the primary 𝑚 1 , secondary 𝑚 2 , and their sum) up to 𝑚 1 + 𝑚 2 35 𝑀 is sensitive to adopted assumption on SN convection growth timescale. Between the two extreme tested variants of convection growth the probability of compact object formation within the lower mass gap may differ up to ∼ 2 orders of magnitude. The distribution of mass ratios of DCO mergers is significantly influenced by SN model only for our standard mass transfer stability criteria for which vast majority of BH-BH mergers are formed through CE phase.

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Section: Discussion Of Caveats and Uncertaintiesmentioning

confidence: 99%

The role of supernova convection for the lower mass gap in the isolated binary formation of gravitational wave sources

Olejak¹,

Fryer²,

Belczyński³

et al. 2022

Preprint

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“…The treatment of mass transfer represents a key source of uncertainty in isolated binary evolution (Belczynski et al 2022). Is the mass transfer dynamically stable?…”

Section: Isolated Binary Evolution With Mass Transfermentioning

confidence: 99%

Rates of compact object coalescences

2022

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Gravitational-wave detections are enabling measurements of the rate of coalescences of binaries composed of two compact objects—neutron stars and/or black holes. The coalescence rate of binaries containing neutron stars is further constrained by electromagnetic observations, including Galactic radio binary pulsars and short gamma-ray bursts. Meanwhile, increasingly sophisticated models of compact objects merging through a variety of evolutionary channels produce a range of theoretically predicted rates. Rapid improvements in instrument sensitivity, along with plans for new and improved surveys, make this an opportune time to summarise the existing observational and theoretical knowledge of compact-binary coalescence rates.

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“…A large number of physical uncertainties embed models of massive-star binary evolution, which have significant impacts on the population properties of their BBH remnants (e.g. Bouffanais et al 2019;Stevenson et al 2019;van Son et al 2020;Bavera et al 2021b;Belczynski et al 2021;Santoliquido et al 2021;. Though recent studies have become increasingly thorough in their coverage of this highly uncertain parameter space (see Broekgaarden et al 2021 for a recent overview), it is computationally expensive and can make interpretation difficult.…”

Section: Physical Assumptionsmentioning

confidence: 99%

Suspicious Siblings: The Distribution of Mass and Spin Across Component Black Holes in Isolated Binary Evolution

Zevin,

Bavera

2022

Preprint

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The LIGO and Virgo gravitational-wave detectors have uncovered systems with definitively nonzero spins, as well as systems with significant spin residing in the heavier black hole of the pair. We investigate the ability of isolated binary evolution in forming such highly spinning, asymmetric mass systems through both accretion onto the first-born black hole and tidal spin-up of the second-born black hole using a rapid population synthesis approach with detailed considerations of spin-up through tidal interactions. Even with the most optimistic assumptions regarding the efficiency at which an accreting star receives material from a donor, we find that it is difficult to form systems with significant mass asymmetry and moderate or high spins in the primary black hole component. Assuming efficient angular momentum transport within massive stars and Eddington-limited accretion onto black holes, we find that < 1.5% of systems in the underlying binary black hole population have a primary black hole spin greater than 0.2 and a mass asymmetry of greater than 2:1 in our most optimistic models, with most models finding that this criteria is only met in ∼ 0.01% of systems. The production of systems with significant mass asymmetries and spin in the primary black hole component is thus an unlikely byproduct of isolated evolution unless highly super-Eddington accretion is invoked or angular momentum transport in massive stars is less efficient than typically assumed.

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The Uncertain Future of Massive Binaries Obscures the Origin of LIGO/Virgo Sources

Cited by 52 publications

References 127 publications

The role of supernova convection for the lower mass gap in the isolated binary formation of gravitational wave sources

The role of supernova convection for the lower mass gap in the isolated binary formation of gravitational wave sources

Rates of compact object coalescences

Suspicious Siblings: The Distribution of Mass and Spin Across Component Black Holes in Isolated Binary Evolution

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