On the Angular Momentum Transport Efficiency within the Star Constrained from Gravitational-wave Observations

Qin, Ying; Wang, Yuan-Zhu; Wu, Dong-Hong; Meynet, Georges; Song, Hanfeng

doi:10.48550/arxiv.2108.04821

Cited by 3 publications

(4 citation statements)

References 32 publications

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“…Binary black hole detections in which the more massive black hole has clearly non-zero spin χ 1 > 0 could be challenging to accommodate in the standard field framework as described above (Mandel & Fragos 2020;Qin et al 2021). Several events in GWTC-2 would seem to fall into this category, including GW151226 (Abbott et al 2016;Chia et al 2021, but see Mateu-Lucena et al 2021, GW190412 (Abbott et al 2020c;Zevin et al 2020, but see Mandel & Fragos 2020, and GW190403 051519 (Abbott et al 2021c;Qin et al 2021, though the high mass already makes field formation unlikely for this system). If these systems formed in the field, it is possible that the more massive black hole formed from what was initially the secondary (lower mass) star that subsequently gained mass through accretion.…”

Section: (2021b)mentioning

confidence: 99%

Building better spin models for merging binary black holes: Evidence for non-spinning and rapidly spinning nearly aligned sub-populations

Galaudage,

Talbot,

Nagar

et al. 2021

Preprint

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Recent work paints a conflicting portrait of the distribution of black hole spins in merging binaries measured with gravitational waves. Some analyses find that a significant fraction of merging binaries contain at least one black hole with a spin tilt > 90 • with respect to the orbital angular momentum vector, which has been interpreted as a signature for dynamical assembly. Other analyses find the data are consistent with a bimodal population in which some binaries contain black holes with negligible spin while the rest contain black holes with spin vectors preferentially aligned with the orbital angular momentum vector. In this work, we scrutinize models for the distribution of black hole spins to pinpoint possible failure modes in which the model yields a faulty conclusion. We reanalyze data from the second LIGO-Virgo gravitational-wave transient catalog (GWTC-2) using a revised spin model, which allows for a sub-population of black holes with negligible spins. In agreement with recent results by Roulet et al., we show that the GWTC-2 detections are consistent with two distinct sub-populations. We estimate that 70 − 90% (90% credible interval) of merging binaries contain black holes with negligible spin χ ≈ 0. The remaining binaries are part of a second sub-population in which the spin vectors are preferentially (but not exactly) aligned to the orbital angular momentum. The black holes in this second sub-population are characterized by spins of χ ∼ 0.5. We suggest that the inferred spin distribution is consistent with the hypothesis that all merging binaries form via the field formation scenario.1. INTRODUCTION Gravitational waves from merging binaries encode information about the mass and spin of the component black holes and/or neutron stars. These properties, in turn, provides clues as to how the binary formed. Two scenarios are frequently invoked to explain merging binary black holes: field and dynamical (see Mandel & Farmer 2018; Mapelli 2021; Mandel & Broekgaarden 2021 for reviews). In the field scenario, binary black hole (BBH) systems are formed from isolated stellar binaries. In the dynamical scenario, BBH systems are assembled through interactions in dense stellar environ-

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Section: (2021b)mentioning

confidence: 99%

Building better spin models for merging binary black holes: Evidence for non-spinning and rapidly spinning nearly aligned sub-populations

Galaudage,

Talbot,

Nagar

et al. 2021

Preprint

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“…Based on GWTC-3, The LIGO Scientific Collaboration et al ( 2021b) have determined that when treating the BHs in BBH systems as the "more and less rapidly spinning components" instead of the more and less massive components of BBH, the more rapidly spinning components have a spin distribution that peaks at a ∼ 0.4, with 1st and 99th percentiles at 0.07 +0.05 −0.03 and 0.8 +0.08 −0.08 , while the less rapidly spinning components have a distribution centered below a ≤ 0.2 and with 99% of values below 0.54 +0.09 −0.08 . Interestingly, Qin et al (2021) report that the most massive of the black holes in the GW190403 051519 event has a dimensionless spin of 0.92 +0.07 −0.22 . While the formation mechanism of BBH is still a topic of debate, the current view is that the entire observed distribution cannot be obtained through a single formation channel (see e.g., Zevin et al 2021).…”

Section: Discussionmentioning

confidence: 99%

The Spin of a Newborn Black Hole: Swift J1728.9-3613

Draghis¹,

Balakrishnan²,

Miller³

et al. 2023

Preprint

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The origin and distribution of stellar-mass black hole spins are a rare window into the progenitor stars and supernova events that create them. Swift J1728.9-3613 is an X-ray binary, likely associated with the supernova remnant G351.9-0.9 (Balakrishnan et al. 2023). A NuSTAR X-ray spectrum of this source during its 2019 outburst reveals reflection from an accretion disk extending to the innermost stable circular orbit. Modeling of the relativistic Doppler shifts and gravitational redshifts imprinted on the spectrum measures a dimensionless spin parameter of a = 0.86 ± 0.02 (1σ confidence), a small inclination angle of the inner accretion disk θ < 10 degrees, and a sub-solar iron abundance in the disk A Fe < 0.84. This high spin value rules out a neutron star primary at the 5 σ level of confidence. If the black hole is located in a still visible supernova remnant, it must be young. Therefore, we place a lower limit on the natal black hole spin of a > 0.82, concluding that the black hole must have formed with a high spin. This demonstrates that black hole formation channels that leave a supernova remnant, and those that do not (e.g. Cyg X-1), can both lead to high natal spin with no requirement for subsequent accretion within the binary system. Emerging disparities between the population of high-spin black holes in X-ray binaries and the low-spin black holes that merge in gravitational wave events may therefore be explained in terms of different stellar conditions prior to collapse, rather than different environmental factors after formation.

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“…For BBHs measured from LIGO/Virgo (Abbott et al 2021), the currently obtained low BH spins are in favor of the efficient angular momentum transport inside massive stars. On the other hand, in order to explain the high spin measurements for BHs in HMXBs, the angular momentum transport has to be inefficient (Qin et al 2019b(Qin et al , 2021. Given the classical isolated formation channel for the two BH binaries, this inconsistency has put a challenge on the angular momentum transport mechanism inside massive stars.…”

Section: Discussionmentioning

confidence: 99%

“…The motivation of this work comes from the inconsistent BH spin measurements in two types of BH binaries (i.e., binary BHs and HMXBs). Such inconsistence has put different constraints on the efficiency of the angular momentum transport inside massive stars in the context of the classical isolated binary evolution channel (Qin et al 2021). Additionally, the measured surface helium abundance of BH companion star is enhanced by more than a factor of two when compared with the solar composition.…”

Section: Introductionmentioning

confidence: 99%

Hypercritical Accretion for Black Hole High Spin in Cygnus X-1

Qin,

Shu,

et al. 2022

Preprint

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Recent observations of AdLIGO and Virgo have shown that the spin measurements in binary black hole (BH) systems are typically small, which is consistent with the predictions by the classical isolated binary evolution channel. In this standard formation channel, the progenitor of the first-born BH is assumed to have efficient angular momentum transport. The BH spins in high-mass X-ray binaries (HMXBs), however, have been found consistently to be extremely high. In order to explain the high BH spins, the inefficient angular momentum transport inside the BH progenitor is required. This requirement, however, is incompatible with the current understanding of conventional efficient angular momentum transport mechanism. We find that this tension can be highly alleviated as long as the hypercritical accretion is allowed. We show that, for a case study of Cygnus X-1, the hypercritical accretion cannot only be a good solution for the inconsistent assumption upon the angular momentum transport within massive stars, but match its other properties reported recently.

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On the Angular Momentum Transport Efficiency within the Star Constrained from Gravitational-wave Observations

Cited by 3 publications

References 32 publications

Building better spin models for merging binary black holes: Evidence for non-spinning and rapidly spinning nearly aligned sub-populations

Building better spin models for merging binary black holes: Evidence for non-spinning and rapidly spinning nearly aligned sub-populations

The Spin of a Newborn Black Hole: Swift J1728.9-3613

Hypercritical Accretion for Black Hole High Spin in Cygnus X-1

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