Binary Black Hole Formation with Detailed Modeling: Stable Mass Transfer Leads to Lower Merger Rates

Gallegos-Garcia, Monica; Berry, C. P. L.; Marchant, Pablo; Kalogera, V.

doi:10.3847/1538-4357/ac2610

Cited by 65 publications

(66 citation statements)

References 154 publications

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“…In some systems the CE may be replaced or preceded by a phase of thermal-timescale stable masstransfer (e.g., Pavlovskii et al 2017;van den Heuvel 2017;Klencki et al 2021;Marchant et al 2021;van Son et al 2021;Bavera et al 2021;Gallegos-Garcia et al 2021), which also has the effect of at least partially tightening the binary on a relatively short timescale (and may leave a relic gaseous disk due to RLOF spillover from the binary during the mass-transfer process; see below).…”

Section: Dynamical Common Envelope Phasementioning

confidence: 99%

Luminous Fast Blue Optical Transients and Type Ibn/Icn SNe from Wolf-Rayet/Black Hole Mergers

Metzger

2022

Preprint

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Progenitor models for the "luminous" subclass of Fast Blue Optical Transients (LFBOTs; prototype: AT2018cow) are challenged to simultaneously explain all of their observed properties: fast optical rise times days; peak luminosities 10 44 erg s −1 ; low yields 0.1M of 56 Ni; aspherical ejecta with a wide velocity range ( 3000 km s −1 to 0.1 − 0.5c with increasing polar latitude); presence of hydrogen-depleted-but-not-free dense circumstellar material (CSM) on radial scales from ∼ 10 14 cm to ∼ 3×10 16 cm; embedded variable source of non-thermal X-ray/γ−rays, suggestive of a compact object. We show that all of these properties are consistent with the tidal disruption and hyper-accretion of a Wolf-Rayet (WR) star by a black hole (BH) or neutron star (NS) binary companion. In contrast with related previous models, the merger occurs with a long delay following the common envelope (CE) event responsible for birthing the binary, as a result of gradual angular momentum loss to a relic circumbinary disk. Disk-wind outflows from the merger-generated accretion flow generate the 56 Nipoor aspherical ejecta with the requisite velocity range. The optical light curve is powered primarily by reprocessing X-rays from the inner accretion flow/jet, though CSM shock interaction also contributes. Primary CSM sources include WR mass-loss from the earliest stages of the merger ( 10 14 cm) and the relic CE disk and its photoevaporation-driven wind ( 10 16 cm). Longer delayed mergers may instead give rise to supernovae Type Ibn/Icn (depending on the WR evolutionary state), connecting these transient classes with LFBOTs.

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Section: Dynamical Common Envelope Phasementioning

confidence: 99%

Luminous Fast Blue Optical Transients and Type Ibn/Icn SNe from Wolf-Rayet/Black Hole Mergers

Metzger

2022

Preprint

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“…A number of formation channels have been put forward to explain the origin of BBH mergers (see Mandel & Broekgaarden 2022 for a review). In the isolated binary evolution channel, compact BH binaries are formed either through common-envelope evolution (e.g., Tutukov & Yungelson 1993;Lipunov et al 1997;Voss & Tauris 2003;Belczynski et al 2016;Eldridge & Stanway 2016;Stevenson et al 2017;Khokhlov et al 2018;Kruckow et al 2018;Spera et al 2019;Breivik et al 2020;Zevin et al 2020;Broekgaarden et al 2021) or through stable mass transfer between the BH and its companion (e.g., van den Heuvel et al 2017;Neijssel et al 2019;Bavera et al 2021;Gallegos-Garcia et al 2021;Shao & Li 2021). Alternatively, merging BHs can be formed via dynamical interactions in globular clusters (Downing et al 2010;Rodriguez et al 2016;Askar et al 2017;Perna et al 2019;Kremer et al 2020) or young stellar clusters (Ziosi et al 2014;Di Carlo et al 2019;Rastello et al 2020;Santoliquido et al 2020;Mapelli et al 2022).…”

Section: Introductionmentioning

confidence: 99%

Stable Mass Transfer Can Explain Massive Binary Black Hole Mergers with a High-spin Component

Shao

2022

ApJ

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Recent gravitational-wave observations showed that binary black hole (BBH) mergers with massive components are more likely to have high effective spins. In the model of isolated binary evolution, BH spins mainly originate from the angular momenta of the collapsing cores before BH formation. Both observations and theories indicate that BHs tend to possess relatively low spins; the origin of fast-spinning BHs remains a puzzle. We investigate an alternative process that stable Case A mass transfer may significantly increase BH spins during the evolution of massive BH binaries. We present detailed binary evolution calculations and find that this process can explain the observed high spins of some massive BBH mergers under the assumption of mildly super-Eddington accretion.

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“…Specifically we are already working on three improvements: (i) in this first version our treatment of the CE phase, once dynamical instability is recognized (taking into account the full stellar structure of the RLO star), is similar to what is done in pBPS codes, apart from the self-consistent calculation of the CE's binding energy. However, since we model binaries with MESA, we are able to treat the phase in a more physical way, either by following the CE inspiral self-consistently using 1D hydrodynamic simulations (e.g., Fragos et al 2019) or by following the long-term response of the RLO star to losing its envelope on a very high rate and have its Roche lobe shrinking rapidly (e.g., Marchant et al 2021b;Gallegos-Garcia et al 2021). One of the objectives of the next version of POSYDON will be to improve the physics of our CE treatment.…”

Section: Summary and Future Workmentioning

confidence: 99%

POSYDON: A General-Purpose Population Synthesis Code with Detailed Binary-Evolution Simulations

Fragos¹,

Andrews²,

Bavera³

et al. 2022

Preprint

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Most massive stars are members of a binary or a higher-order stellar systems, where the presence of a binary companion can decisively alter their evolution via binary interactions. Interacting binaries are also important astrophysical laboratories for the study of compact objects. Binary population synthesis studies have been used extensively over the last two decades to interpret observations of compact-object binaries and to decipher the physical processes that lead to their formation. Here, we present POSYDON, a novel , binary population synthesis code that incorporates full stellar-structure and binary-evolution modeling, using the MESA code, throughout the whole evolution of the binaries. The use of POSYDON enables the self-consistent treatment of physical processes in stellar and binary evolution, including: realistic mass-transfer calculations and assessment of stability, internal angularmomentum transport and tides, stellar core sizes, mass-transfer rates and orbital periods. This paper describes the detailed methodology and implementation of POSYDON, including the assumed physics of stellar-and binary-evolution, the extensive grids of detailed single-and binary-star models, the post-processing, classification and interpolation methods we developed for use with the grids, and the treatment of evolutionary phases that are not based on pre-calculated grids. The first version of POSYDON targets binaries with massive primary stars (potential progenitors of neutron stars or black holes) at solar metallicity.

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Binary Black Hole Formation with Detailed Modeling: Stable Mass Transfer Leads to Lower Merger Rates

Cited by 65 publications

References 154 publications

Luminous Fast Blue Optical Transients and Type Ibn/Icn SNe from Wolf-Rayet/Black Hole Mergers

Luminous Fast Blue Optical Transients and Type Ibn/Icn SNe from Wolf-Rayet/Black Hole Mergers

Stable Mass Transfer Can Explain Massive Binary Black Hole Mergers with a High-spin Component

POSYDON: A General-Purpose Population Synthesis Code with Detailed Binary-Evolution Simulations

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