Evaluating chemically homogeneous evolution in stellar binaries: electromagnetic implications – ionizing photons, SLSN-I, GRB, Ic-BL

Ghodla, Sohan; Eldridge, J. J.; Stanway, Elizabeth R.; Stevance, H. F.

doi:10.1093/mnras/stac3177

Cited by 13 publications

(9 citation statements)

References 124 publications

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“…Here, M, r g , and v cr are the pre-accretion mass, radius of gyration, and the critical velocity of the star, respectively, and it is assumed that the star is rotating as a solid body. This expression has been adopted from Ghodla et al ( 2023 ), who studied the spin-up efficiency in the secondary component of a binary system due to accretion of mass from a Keplerian disc around the accretor. Since the projection of the VFTS 243 orbit is unknown, we allow all velocities larger than 180 km s −1 (up to critical) in our working.…”

Section: O D E L S a N D N U M E R I C A L M E T H O D Smentioning

confidence: 99%

VFTS 243 as predicted by the BPASS fiducial models

Stevance

Ghodla

Richards

et al. 2023

Monthly Notices of the Royal Astronomical Society

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The recent discovery of an unambiguous quiescent BH and main sequence O star companion in VFTS 243 opens the door to new constraints on theoretical stellar evolution and population models looking to reproduce the progenitors of black hole - black hole binaries. Here we show that the Binary Population and Spectral Synthesis fiducial models (BPASSv2.2.1) natively predict VFTS 243-like systems: We find that VFTS 243 likely originated from a binary system in a ∼15 day orbit with primary mass ranging from 40 to 50 M⊙ and secondary star with initial mass 24–25 M⊙. Additionally we find that the death of the primary star must have resulted in a low energy explosion E < 1050 ergs. With a uniform prior we find that the kick velocity of the new-born black hole was ≤10 km s−1. The very low eccentricity reported for VFTS 243 and the subsequent conclusion by the authors that the SN kick must have been very small is in line with the peak in the posterior distribution between 0 and 5 km s−1 found from our numerical simulations performed with a uniform prior. Finally, the reduced Hobbs kick distribution commonly used in black hole population synthesis is strongly disfavoured, whereas the Bray kick with the most recent parameter calibration predicts 4.2 ± 3.4 km s−1, which is very consistent with the posterior velocity distributions obtained for our matching VFTS 243-like models using a uniform kick prior.

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Section: O D E L S a N D N U M E R I C A L M E T H O D Smentioning

confidence: 99%

VFTS 243 as predicted by the BPASS fiducial models

Stevance

Ghodla

Richards

et al. 2023

Monthly Notices of the Royal Astronomical Society

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“…This makes the CHE pathway of interest as a formation pathway for gravitational-wave sources, as initially suggested independently by and Marchant et al (2016). 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: 88%

“…CHE has also been considered in the case of very rapidly rotating single stars, where mixing processes resulting from rotation may be responsible for keeping the stars homogeneous (Maeder & Meynet 1987;Yoon et al 2006;Brott et al 2011). In wider binaries, CHE may also occur for the mass-gaining star that is spun up as a result of accretion (e.g., Cantiello et al 2007;de Mink et al 2013;Ghodla et al 2023). In our work, we will refer to these as "birth-spin CHE" and "accretion-induced CHE," respectively, to distinguish them from "tidal CHE" as described in the previous paragraph.…”

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

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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.

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“…Alternatively, the CHE induced by the accretion from its companion could also be reached for massive stars with weak tidal interactions in relatively wide orbits (Cantiello et al 2007). Recently, Ghodla et al (2023) claimed that the accretion-induced CHE could be an important formation channel producing electromagnetic transients like GRBs/Ic-BL (SLSN-I/Ic-BL) 14 under the collapsar (magnetar) scenario. In addition to CEE and SMT, the CHE was also found to play a critical role in contributing to the long GRB rate (Bavera et al 2022c).…”

Section: Properties Of Bbhs Predicted By the Che Channelmentioning

confidence: 99%

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

Qin

Wang

Bavera

et al. 2022

ApJ

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The LIGO, Virgo, and KAGRA (LVK) Collaboration has announced 90 coalescing binary black holes (BBHs) with p astro > 50% to date; however, the origin of their formation channels is still an open scientific question. Given various properties of BBHs (BH component masses and individual spins) inferred using the default priors by the LVK, independent groups have been trying to explain the formation of the BBHs with different formation channels. Of all formation scenarios, the chemically homogeneous evolution (CHE) channel has stood out with distinguishing features, namely, nearly equal component masses and preferentially high individual spins aligned with the orbital angular momentum. We perform Bayesian inference on the BBH events officially reported in GWTC-3 with astrophysically predicted priors representing different formation channels of the isolated binary evolution (common-envelope evolution channel, CEE; CHE; stable mass transfer, SMT). Given assumed models, we report strong evidence for GW190517_055101 being most likely to have formed through the CHE channel. Assuming the BBH events in the subsample are all formed through one of the isolated binary evolution channels, we obtain the lower limits on the local merger rate density of these channels at 11.45 Gpc−3 yr−1 (CEE), 0.18 Gpc−3 yr−1 (CHE), and 0.63 Gpc−3 yr−1 (SMT) at 90% credible level.

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Evaluating chemically homogeneous evolution in stellar binaries: electromagnetic implications – ionizing photons, SLSN-I, GRB, Ic-BL

Cited by 13 publications

References 124 publications

VFTS 243 as predicted by the BPASS fiducial models

VFTS 243 as predicted by the BPASS fiducial models

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

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

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