Tossing Black Hole Spin Axes

Tauris, T. M.

doi:10.3847/1538-4357/ac86c8

Cited by 14 publications

(6 citation statements)

References 83 publications

(107 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…That allows to derive a distribution dominated by low BH spins, with an appropriate fraction of highspinning BHs. Tauris (2022) has additionally considered the effect of BH spin-axis tossing in their isolated binary evolution model. Trani et al (2021), on the other hand, have demonstrated that an LVK-like symmetry breaking can as well occur solely due to misalignments introduced to BBHs (derived from interacting star-star binaries) via dynamical binary-single encounters inside young star clusters.…”

Section: Introductionmentioning

confidence: 99%

Merger rate density of stellar-mass binary black holes from young massive clusters, open clusters, and isolated binaries: Comparisons with LIGO-Virgo-KAGRA results

Banerjee

2022

Phys. Rev. D

View full text Add to dashboard Cite

Properties of the to-date-observed binary black hole (BBH) merger events suggest a preference towards spin-orbit aligned mergers. Naturally, this has caused widespread interest and speculations regrading implications on various merger formation channels. Here we show that (i) not only the BBHmerger population from isolated binaries, but also (ii) BBH population formed in young massive clusters (YMC) would possess an asymmetry in favour of aligned mergers, in the distribution of the events' effective spin parameter (χ eff ). In our analysis, we utilize BBH-merger outcomes from state-of-the-art N-body evolutionary models of YMCs and isolated binary population synthesis. We incorporate, for the first time in such an analysis, misalignments due to both natal kicks and dynamical encounters. The YMC χ eff distribution has a mean (an anti-aligned merger fraction) of χ eff ≤ 0.05 (f X − ≈ 40%) which is smaller (larger) than but consistent with the observed asymmetry of χ eff ≈ 0.06 (f X − ≈ 28%). In contrast, isolated binaries alone tend to produce a much stronger asymmetry; for the tested physical models, χ eff ≈ 0.25 and f X − 7%. Although the YMC χ eff distribution is more similar to the observed counterpart, none of the channels correctly reproduce the observed distribution. Our results suggest that further extensive model explorations for both isolated-binary and dynamical channels as well as better observational constraints are necessary to understand the physics of 'the symmetry breaking' of the BBH-merger population.

show abstract

Section: Introductionmentioning

confidence: 99%

Merger rate density of stellar-mass binary black holes from young massive clusters, open clusters, and isolated binaries: Comparisons with LIGO-Virgo-KAGRA results

Banerjee

2022

Phys. Rev. D

View full text Add to dashboard Cite

show abstract

“…Alternatively, Cyg X-1 may still be a member of the OB3 association, but the maximum asymmetric natal kick could be higher than the assumed (MJ21) 10-20 km s −1 . In fact, a recent study (Tauris 2022) has shown that the observed distribution of inspiral spins of merging BHs, showing a strong tail of negative values, is in clear tension with the current theoretical models of binary evolution and supernovae. Tauris (2022) showed that the discrepancy can be resolved if some BHs have their spins tossed in a random direction during their formation and proposed some tentative mechanisms for the tossing.…”

Section: Discussionmentioning

confidence: 82%

Evidence for a Black Hole Spin–Orbit Misalignment in the X-Ray Binary Cyg X-1

Zdziarski

Veledina

Szanecki

et al. 2023

ApJL

View full text Add to dashboard Cite

Recently, the accretion geometry of the black hole X-ray binary Cyg X-1 was probed with the X-ray polarization. The position angle of the X-ray-emitting flow was found to be aligned with the position angle of the radio jet in the plane of the sky. At the same time, the observed high polarization degree could be obtained only for a high inclination of the X-ray-emitting flow, indicating a misalignment between the binary axis and the black hole spin. The jet, in turn, is believed to be directed by the spin axis; hence, a similar misalignment is expected between the jet and binary axes. We test this hypothesis using very long (up to about 26 yr) multiband radio observations. We find a misalignment of 20°–30°. However, contrary to the earlier expectations, the jet and binary viewing angles are found to be similar, while the misalignment is seen between the position angles of the jet and the binary axis on the plane of the sky. Furthermore, the presence of the misalignment calls into question our understanding of the evolution of this binary system.

show abstract

“…Finally, the model used in this work (and the Default spin model in Abbott et al 2021d) assumes that these are the only two categories of spin-direction distributions: isotropic binaries originating in the field and aligned binaries originating in dense stellar clusters. However, the spin axis of BHs evolving in isolation can change direction during the core collapse of a star, potentially resulting in an isotropic-spin distribution for the first-born BH (Farr et al 2011;Tauris 2022). Moreover, formation scenarios-such as BBHs synthesized in AGN disks -might predict a binary where one or both BH spins are antialigned with orbital angular momentum (McKernan et al 2020;Tagawa et al 2020).…”

Section: Caveatsmentioning

confidence: 99%

Dropping Anchor: Understanding the Populations of Binary Black Holes with Random and Aligned-spin Orientations

Baibhav

Doctor

Kalogera

2023

ApJ

View full text Add to dashboard Cite

The relative spin orientations of black holes (BHs) in binaries encode their evolutionary history: BHs assembled dynamically should have isotropically distributed spins, while spins of BHs originating in the field should be aligned with the orbital angular momentum. In this article, we introduce a simple population model for these dynamical and field binaries that uses spin orientations as an anchor to disentangle these two evolutionary channels. We then analyze binary BH mergers in the Third Gravitational-Wave Transient Catalog (GWTC-3) and ask whether BHs from the isotropic-spin population possess different distributions of mass ratios, spin magnitudes, or redshifts from the preferentially aligned-spin population. We find no compelling evidence that binary BHs in GWTC-3 have different source-property distributions depending on their spin alignment, but we do find that the dynamical and field channels cannot both have mass-ratio distributions that strongly favor equal masses. We give an example of how this can be used to provide insights into the various processes that drive these BHs to merge. We also find that the current detections are insufficient in extracting differences in spin magnitude or redshift distributions of isotropic and aligned-spin populations.

show abstract

Tossing Black Hole Spin Axes

Cited by 14 publications

References 83 publications

Merger rate density of stellar-mass binary black holes from young massive clusters, open clusters, and isolated binaries: Comparisons with LIGO-Virgo-KAGRA results

Merger rate density of stellar-mass binary black holes from young massive clusters, open clusters, and isolated binaries: Comparisons with LIGO-Virgo-KAGRA results

Evidence for a Black Hole Spin–Orbit Misalignment in the X-Ray Binary Cyg X-1

Dropping Anchor: Understanding the Populations of Binary Black Holes with Random and Aligned-spin Orientations

Contact Info

Product

Resources

About