Searching for Candidates of Coalescing Binary Black Holes Formed through Chemically Homogeneous Evolution in GWTC-3

Qin, Ying; Wang, Yuan-Zhu; Bavera, Simone S.; Wu, Shichao; Meynet, Georges; Wang, Yiying; Hu, Rui-Chong; Zhu, Jinwei; Dong-Hong, Wu,; Shu, Xinwen; Peng, Fang‐Kun; Song, Hongwen; Wei, Da-Ming

doi:10.3847/1538-4357/aca40c

“…Alternatively, predicted distributions from each channel can be used to infer individually what is the likelihood that a single source is produced by a specific formation scenario (e.g. Qin et al 2022;Antonelli et al 2023). However, conclusions from model comparison can be severely affected if one lacks knowledge of some formation channels (Qiu Cheng et al 2023), and predicted distributions have large uncertainties with different codes predicting drastically different outcomes even for individual binary systems (e.g.…”

Section: Introductionmentioning

confidence: 99%

The role of mass transfer and common envelope evolution in the formation of merging binary black holes

Marchant

¹

,

Pappas

²

,

Gallegos-Garcia

³

et al. 2021

A&A

View full text Add to dashboard Cite

As the number of merging binary black holes observed with ground-based gravitational-wave detectors grows, increasingly accurate theoretical models are required to compare them to the observed sample and disentangle contributions from multiple channels. In formation models involving isolated binary stars, important uncertainties remain regarding the stability of mass transfer and common-envelope evolution. To study some of these uncertainties, we have computed binary simulations using the MESA code consisting of a 30 M⊙ star in a low metallicity (Z⊙/10) environment with a black-hole companion. We have developed an updated prescription to compute mass transfer rates including the possibility of outflows from outer Lagrangian points, as well as a method to self-consistently determine the core-envelope boundary in cases where there is common-envelope evolution. We find that binaries survive common-envelope evolution only if unstable mass transfer happens after the formation of a deep convective envelope, resulting in a narrow range (0.2 dex) in period for successful envelope ejection. All cases where binary interaction is initiated with a radiative envelope have large binding energies (∼1050 erg), and they result in mergers during the common-envelope phase even under the assumption that all the internal and recombination energy of the envelope, as well as the energy from an inspiral, is used to eject the envelope. This is independent of whether or not helium is ignited in the core of the donor, conditions under which various rapid-population synthesis calculations assume a successful envelope ejection is possible. Moreover, we find that the critical mass ratio for instability is such that across a large range in initial orbital periods (∼1−1000 days), merging binary black holes can be formed via stable mass transfer. A large fraction of these systems undergo overflow of their L2 equipotential, in which case we find that stable mass transfer produces merging binary black holes even under extreme assumptions of mass and angular momentum outflows. Our conclusions are limited to the study of one donor mass at a single metallicity, but they suggest that population synthesis calculations overestimate the formation rate of merging binary black holes produced by common-envelope evolution and that stable mass transfer could dominate the formation rate from isolated binaries. This is in agreement with a few other recent studies. Further work is required to extend these results to different masses and metallicities as well as to understand how they can be incorporated into rapid population synthesis calculations.

show abstract

“…In Paper I, we carried out detailed binary modeling to investigate this peculiar channel, mainly focusing on the properties of resulting BHs and their associated tidal disruption probabilities (see also Chattopadhyay et al 2021;Román-Garza et al 2021). Alternatively, the immediate progenitor of the BHNS binary could be a BH-He-rich star system formed after the CE phase or through chemically homogeneous evolution (de Mink Mandel & de Mink 2016;Marchant et al 2016;Song et al 2016;du Buisson et al 2020;Riley et al 2021;Zevin et al 2021;Bavera et al 2022aBavera et al , 2022bQin et al 2022c). The BH can be spun up via the accretion during the stable MT phase (see the recent studies, Qin et al 2022a;Shao & Li 2022;Zevin & Bavera 2022;Steinle et al 2023), called accretion-induced spin-up.…”

Section: Introductionmentioning

confidence: 99%

A Channel to Form Fast-spinning Black Hole–Neutron Star Binary Mergers as Multimessenger Sources. II. Accretion-induced Spin-up

Wang,

Hu,

Qin

et al. 2024

ApJ

Self Cite

2

0

View full text Add to dashboard Cite

In this work, we investigate an alternative channel for the formation of fast-spinning black hole–neutron star (BHNS) binaries, in which super-Eddington accretion is expected to occur in accreting BHs during the stable mass transfer phase within BH-stripped helium (BH–He-rich) star binary systems. We evolve intensive MESA grids of close-orbit BH–He-rich star systems to systematically explore the projected aligned spins of BHs in BHNS binaries, as well as the impact of different accretion limits on the tidal disruption probability and electromagnetic (EM) signature of BHNS mergers. Most of the BHs in BHNS mergers cannot be effectively spun up through accretion if the accretion rate is limited to ≲ 10 M ̇ Edd , where M ̇ Edd is the standard Eddington accretion limit. In order to reach high spins (e.g., χ BH ≳ 0.5), the BHs are required to be born less massive (e.g., ≲3.0 M ⊙) in binary systems with initial periods of ≲0.2–0.3 days and accrete material at ∼ 100 M ̇ Edd . However, even under this high accretion limit, ≳6 M ⊙ BHs are typically challenging to significantly spin up and generate detectable associated EM signals. Our population simulations suggest that different accretion limits have a slight impact on the ratio of tidal disruption events. However, as the accretion limit increases, the EM counterparts from the cosmological BHNS population can become bright overall.

show abstract

“…Since then, several studies have further explored this pathway (de Mink & Mandel 2016; Marchant et al 2017;du Buisson et al 2020;Riley et al 2021;Ghodla et al 2023;Dorozsmai et al 2024). Some studies even suggest that certain observed gravitational-wave sources show significant support for a CHE origin (Qin et al 2022).…”

Section: Introductionmentioning

confidence: 99%

Investigating the Chemically Homogeneous Evolution Channel and Its Role in the Formation of the Enigmatic Binary Black Hole Progenitor Candidate HD 5980

Sharpe,

van Son,

de Mink

et al. 2024

ApJ

0

View full text Add to dashboard Cite

Chemically homogeneous evolution (CHE) is a promising channel for forming massive binary black holes. The enigmatic, massive Wolf–Rayet binary HD 5980 A&B has been proposed to have formed through this channel. We investigate this claim by comparing its observed parameters with CHE models. Using MESA, we simulate grids of close massive binaries, then use a Bayesian approach to compare them with the stars’ observed orbital period, masses, luminosities, and hydrogen surface abundances. The most probable models, given the observational data, have initial periods ∼3 days, widening to the present-day ∼20 days orbit as a result of mass loss—correspondingly, they have very high initial stellar masses (≳150 M ⊙). We explore variations in stellar-wind mass loss and internal mixing efficiency, and find that models assuming enhanced mass loss are greatly favored to explain HD 5980, while enhanced mixing is only slightly favored over our fiducial assumptions. Our most probable models slightly underpredict the hydrogen surface abundances. Regardless of its prior history, this system is a likely binary black hole progenitor. We model its further evolution under our fiducial and enhanced wind assumptions, finding that both stars produce black holes with masses ∼19–37 M ⊙. The projected final orbit is too wide to merge within a Hubble time through gravitational waves alone. However, the system is thought to be part of a 2+2 hierarchical multiple. We speculate that secular effects with the (possible) third and fourth companions may drive the system to promptly become a gravitational-wave source.

show abstract

Searching for Candidates of Coalescing Binary Black Holes Formed through Chemically Homogeneous Evolution in GWTC-3

Cited by 6 publications

References 98 publications

The role of mass transfer and common envelope evolution in the formation of merging binary black holes

The role of mass transfer and common envelope evolution in the formation of merging binary black holes

A Channel to Form Fast-spinning Black Hole–Neutron Star Binary Mergers as Multimessenger Sources. II. Accretion-induced Spin-up

Investigating the Chemically Homogeneous Evolution Channel and Its Role in the Formation of the Enigmatic Binary Black Hole Progenitor Candidate HD 5980

Contact Info

Product

Resources

About