The formation of merging black holes with masses beyond 30 M⊙ at solar metallicity

Bavera, Simone S.; Fragos, Tassos; Zapartas, Emmanouil; Andrews, Jeff J.; Kalogera, V.; Berry, C. P. L.; Kruckow, Matthias U.; Dotter, Aaron; Kovlakas, Konstantinos; Misra, Devina; Rocha, Kyle A.; Srivastava, Philipp M.; Sun, Meng; Xing, Zepei

doi:10.1038/s41550-023-02018-5

Cited by 11 publications

(6 citation statements)

References 68 publications

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“…In contrast with other models like Bavera et al (2023) we do not report a quasi-flat distribution of BH masses for the most massive stars in our models, nor a BH mass peak in the lowmass range. On the contrary, the BH mass increases monotonically as a function of ZAMS mass to M BH = 27.7 M e for our most massive model at M ZAMS = 300 M e .…”

Section: Resultscontrasting

confidence: 99%

“…We find a different initial-final star mass relation for our updated stellar models. First, our models predict a maximum BH mass of ∼28 M e that is smaller by at least ∼7 M e if compared to Bavera et al (2023) and Martinet et al (2023). Second, our most massive BHs are formed from significantly different initial star masses (M ZAMS > 250 M e ) than the ones found by Bavera et al (2023) from single star evolution (M ZAMS ∼ 75 M e ).…”

Section: Discussionmentioning

confidence: 61%

“…Yet, for the two test models (at M ZAMS = 60 and 200 M e ) both codes produce almost identical final star masses that show robustness of our predictions. We also show as a comparison the estimates from Martinet et al (2023) and an approximation of the BH mass distribution from Bavera et al (2023). Most of the stars in our models, according to Fryer et al (2012), collapse directly into BHs without any supernova event.…”

Section: Resultsmentioning

confidence: 84%

“…The final star mass may be taken as a proxy for BH mass (direct BH formation) or as an upper limit on BH mass (if there is a supernova explosion involved in the BH formation). First, Bavera et al (2023) performed stellar evolution of massive stars (both as single stars and as parts of a binary system) in the zero-age main-sequence (ZAMS) star mass range M ZAMS = 15-150 M e at Z = 0.014 with the MESA evolutionary code. They found that the BH mass from single star evolution increases from M BH = 3 M e at M ZAMS = 15 M e to a peak value at M BH = 35 M e at M ZAMS = 75 M e , and then BH mass rapidly decreases with initial mass to M BH = 15 M e at M ZAMS = 100 M e .…”

Section: Introductionmentioning

confidence: 99%

“…We take advantage of these new results to update our calculations. Additionally, in Bavera et al (2023) only nonrotating models were used, and in Martinet et al (2023) a rather modest overshooting was employed (α ov ∼ 0.2).…”

Section: Introductionmentioning

confidence: 99%

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On the Maximum Black Hole Mass at Solar Metallicity

Romagnolo,

Gormaz-Matamala,

Belczynski

2024

ApJL

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In high-metallicity environments the mass that black holes (BHs) can reach just after core collapse widely depends on how much mass their progenitor stars lose via winds. On one hand, new theoretical and observational insights suggest that early-stage winds should be weaker than what many canonical models prescribe. On the other hand, the proximity to the Eddington limit should affect the formation of optically thick envelopes already during the earliest stages of stars with initial masses M ZAMS ≳ 100 M ⊙, hence resulting in higher mass-loss rates during the main sequence. We use the evolutionary codes MESA and Genec to calculate a suite of tracks for massive stars at solar metallicity Z ⊙ = 0.014, which incorporate these changes in our wind-mass-loss prescription. In our calculations we employ moderate rotation, high overshooting, and magnetic angular momentum transport. We find a maximum BH mass M BH , max = 28.3 M ⊙ at Z ⊙. The most massive BHs are predicted to form from stars with M ZAMS ≳ 250 M ⊙, with the BH mass directly proportional to its progenitor’s M ZAMS. We also find in our models that at Z ⊙ almost any BH progenitor naturally evolves into a Wolf–Rayet star due to the combined effect of internal mixing and wind mass loss. These results are considerably different from most recent studies regarding the final mass of stars before their collapse into BHs. While we acknowledge the inherent uncertainties in stellar evolution modeling, our study underscores the importance of employing the most up-to-date physics in BH mass predictions.

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Section: Resultscontrasting

confidence: 99%

Section: Discussionmentioning

confidence: 61%

Section: Resultsmentioning

confidence: 84%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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On the Maximum Black Hole Mass at Solar Metallicity

Romagnolo,

Gormaz-Matamala,

Belczynski

2024

ApJL

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Compact objects in close orbits as gravitational wave sources: Formation scenarios and properties

Li,

Chen

2024

Results in Physics

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From ZAMS to merger: Detailed binary evolution models of coalescing neutron star – black hole systems at solar metallicity

Xing,

Bavera,

Fragos

et al. 2024

A&A

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Neutron star -- black hole (NSBH) merger events bring us new opportunities to constrain theories of stellar and binary evolution and understand the nature of compact objects. In this work, we investigated the formation of merging NSBH binaries at solar metallicity by performing a binary population synthesis study of merging NSBH binaries with the newly developed code POSYDON sun sun $. Independently of our model variations, the BH always forms first with dimensionless spin parameter $ 0.2$, which is correlated to the initial binary orbital period. Some BHs can subsequently spin up moderately ($ BH 0.4$) due to mass transfer, which we assume to be Eddington limited. Binaries that experience CE evolution rarely demonstrate large tilt angles. Conversely, approximately $40<!PCT!>$ of the binaries that undergo only stable mass transfer without CE evolution contain an anti-aligned BH. Finally, accounting for uncertainties in both the population modeling and the NS equation of state, we find that $0-18.6<!PCT!>$ of NSBH mergers may be accompanied by an electromagnetic counterpart.

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The formation of merging black holes with masses beyond 30 M⊙ at solar metallicity

Cited by 11 publications

References 68 publications

On the Maximum Black Hole Mass at Solar Metallicity

On the Maximum Black Hole Mass at Solar Metallicity

Compact objects in close orbits as gravitational wave sources: Formation scenarios and properties

From ZAMS to merger: Detailed binary evolution models of coalescing neutron star – black hole systems at solar metallicity

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