Re-estimating the Spin Parameter of the Black Hole in Cygnus X-1

Zhao, Xueshan; Gou, Lijun; Dong, Yanting; Zheng, X.; Steiner, James F.; Miller-Jones, J. C. A.; Bahramian, A.; Orosz, Jerome A.; Feng, Ye

doi:10.3847/1538-4357/abbcd6

Cited by 48 publications

(38 citation statements)

References 70 publications

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“…Other pathways to fastspinning BH progenitor stars, in single or binary systems, have been proposed to lead to LGRBs (e.g., Yoon et al 2006;Cantiello et al 2007), albeit none at a rate that matches the observed one when considering efficient AM transport in stellar interiors (Fryer et al 2007). Observed high-mass X-ray binaries that contain fast-spinning BHs, such as Cygnus X-1 (e.g., Gou et al 2011;Zhao et al 2021), may have also been progenitors of LGRBs. The formation of these systems is puzzling (e.g., Wong et al 2012;Neijssel et al 2021), and it is uncertain whether the BH spin in these systems originates from fast-spinning pre-collapse cores (see, e.g., Moreno Méndez et al 2008;Batta et al 2017;Schrøder et al 2018).…”

Section: Discussionmentioning

confidence: 99%

Probing the progenitors of spinning binary black-hole mergers with long gamma-ray bursts

Bavera

Fragos

Zapartas

et al. 2022

A&A

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Long-duration gamma-ray bursts are thought to be associated with the core-collapse of massive, rapidly spinning stars and the formation of black holes. However, efficient angular momentum transport in stellar interiors, currently supported by asteroseismic and gravitational-wave constraints, leads to predominantly slowly-spinning stellar cores. Here, we report on binary stellar evolution and population synthesis calculations, showing that tidal interactions in close binaries not only can explain the observed subpopulation of spinning, merging binary black holes but also lead to long gamma-ray bursts at the time of black-hole formation. Given our model calibration against the distribution of isotropic-equivalent energies of luminous long gamma-ray bursts, we find that ≈10% of the GWTC-2 reported binary black holes had a luminous long gamma-ray burst associated with their formation, with GW190517 and GW190719 having a probability of ≈85% and ≈60%, respectively, being among them. Moreover, given an assumption about their average beaming fraction, our model predicts the rate density of long gamma-ray bursts, as a function of redshift, originating from this channel. For a constant beaming fraction fB ∼ 0.05 our model predicts a rate density comparable to the observed one, throughout the redshift range, while, at redshift z ∈ [0, 2.5], a tentative comparison with the metallicity distribution of observed LGRB host galaxies implies that between 20% to 85% of the observed long gamma-ray bursts may originate from progenitors of merging binary black holes. The proposed link between a potentially significant fraction of observed, luminous long gamma-ray bursts and the progenitors of spinning binary black-hole mergers allows us to probe the latter well outside the horizon of current-generation gravitational wave observatories, and out to cosmological distances.

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Section: Discussionmentioning

confidence: 99%

Probing the progenitors of spinning binary black-hole mergers with long gamma-ray bursts

Bavera

Fragos

Zapartas

et al. 2022

A&A

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“…The primary in GW200115 may even have relatively high spin, with a 90% upper limit of 0.72. Several studies of the observed population of high-mass X-ray binaries (Liu et al 2008;Gou et al 2009Gou et al , 2014Zhao et al 2021) find that the BHs have large spins (Valsecchi et al 2010;Wong et al 2012;Qin et al 2019;Zhao et al 2021). Given the short lifetime of the secondary, mass transfer is argued to be insufficient to generate BHs with such high spins, implying that the BHs were born with high spins.…”

Section: Spinsmentioning

confidence: 99%

Observation of Gravitational Waves from Two Neutron Star–Black Hole Coalescences

Abbott

Abraham

et al. 2021

ApJL

613

334

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We report the observation of gravitational waves from two compact binary coalescences in LIGO's and Virgo's third observing run with properties consistent with neutron star-black hole (NSBH) binaries. The two events are named GW200105_162426 and GW200115_042309, abbreviated as GW200105 and GW200115; the first was observed by LIGO Livingston and Virgo and the second by all three LIGO-Virgo detectors. The source of GW200105 has component masses -+ 8.9 1.5 1.2 and 130 Gpc yr 69 112 3 1 under the assumption of a broader distribution of component masses.

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“…The BH mass, the inclination and the distance of the system was estimated to be 21.2±2.2 M ⊙ , 27.51°+ 0.77 −0.57 , and 2.22 +0.18 −0.17 kpc using VLBA observations (Miller-Jones et al 2021). The dimensionless spin parameter of the BH a * was estimated as ∼ 0.998 (Zhao et al 2021;Kushwaha et al 2021).…”

Section: Introductionmentioning

confidence: 99%

“…Cyg X-1 exhibits one of the best established examples of relativistic reflection study, especially in the soft state (Duro et al 2011;Fabian et al 2012). Many studies on Xray reflection of Cyg X-1 have constrained the characteristic properties of the system such as the Fe abundance of the disk, the inner disk radius or the spin of the BH (Zhao et al 2021;Walton et al 2016;Tomsick et al 2014;Basak et al 2017).…”

Section: Introductionmentioning

confidence: 99%

Evolution of Accretion Modes between Spectral States Inferred from Spectral and Timing Analysis of Cygnus X-1 with Insight-HXMT observations

Feng,

Kong,

Wang

et al. 2022

Preprint

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We execute a detailed spectral-timing study of Cygnus X-1 in the low/hard, intermediate and high/soft states with the Hard X-ray Modulation Telescope observations. The broad band energy spectra show that the disk truncates at a radius related to the spectral state as well as the input spin and inclination parameters. Given a * =0.9696 and i=42.47°, the inner boundary of the disk stays quite close to the ISCO and moves inward slightly as the source softens. Through studying of PDS, rms and Fourier-frequency component resolved spectroscopy of the three typical states, we find that the X-ray variations are generated in two different regions. We discover that the major role that contributes to the X-ray variation is the hot corona rather than the accretion disk. We suggest a scenario with different corona geometry for each state based on the truncated disk geometry in which the corona wraps up the disk to form a sandwich geometry in the low/hard state, and then gradually moves away from the disk in direction that is perpendicular to the disk until forming a lamppost-like geometry in the high/soft state.

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Re-estimating the Spin Parameter of the Black Hole in Cygnus X-1

Cited by 48 publications

References 70 publications

Probing the progenitors of spinning binary black-hole mergers with long gamma-ray bursts

Probing the progenitors of spinning binary black-hole mergers with long gamma-ray bursts

Observation of Gravitational Waves from Two Neutron Star–Black Hole Coalescences

Evolution of Accretion Modes between Spectral States Inferred from Spectral and Timing Analysis of Cygnus X-1 with Insight-HXMT observations

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