A noninteracting low-mass black hole–giant star binary system

Thompson, Todd A.; Kochanek, C. S.; Stanek, K. Z.; Badenes, Carles; Post, R. S.; Jayasinghe, T.; Latham, David W.; Bieryla, Allyson; Esquerdo, Gilbert A.; Berlind, P.; Calkins, M.; Tayar, Jamie; Lindegren, L.; Johnson, Jennifer A.; Holoien, T. W. S.; Auchettl, Katie; Covey, Kevin R.

doi:10.1126/science.aau4005

Cited by 298 publications

(235 citation statements)

References 83 publications

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“…This system is one of the widest known binary system hosting a stellarorigin BH, see https://stellarcollapse.org. Two other binaries, proposed to host BH candidates, were also discovered by the radial velocity method by Thompson et al (2019) and Giesers et al (2018, although this is in a globular cluster and has a very large period, P = 167 d, and eccentric orbit with e = 0.6 and it must have formed by capture).…”

Section: Introductionmentioning

confidence: 94%

The Formation of a 70 M_⊙ Black Hole at High Metallicity

Belczyński

Hirschi

Kaiser

et al. 2020

ApJ

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A 70 M black hole was discovered in Milky Way disk in a long period (P = 78.9 days) and almost circular (e = 0.03) detached binary system (LB-1) with a high (Z ∼ 0.02) metallicity 8 M B star companion. Current consensus on the formation of black holes from high metallicity stars limits the black hole mass to be below 20 M due to strong mass loss in stellar winds. So far this was supported by the population of Galactic black hole X-ray binaries with Cyg X-1 hosting the most massive ∼ 15 M black hole. Using the Hurley et al. 2000 analytic evolutionary formulae, we show that the formation of a 70 M black hole in high metallicity environment is possible if stellar wind mass loss rates, that are typically adopted in evolutionary calculations, are reduced by factor of 5.As observations indicate, a fraction of massive stars (∼ 7%) have surface magnetic fields which, as suggested by Owocki et al. 2016, may quench the wind mass-loss, independently of stellar mass and metallicity. We also computed detailed stellar evolution models and we confirm such a scenario. A non-rotating 85 M star model at Z = 0.014 with decreased winds ends up as a 71 M star prior corecollapse with a 32 M helium core and a 28 M CO core. Such star avoids pair-instability pulsation supernova mass loss that severely limits black hole mass and may form a ∼ 70 M black hole in the direct collapse. Stars that can form 70 M black holes at high Z expand to significant size with radius of R 600 R (thanks to large H-rich envelope), however, exceeding the size of LB-1 orbit (semi-major axis a 350 R ). Therefore, we can explain the formation of black holes upto 70 M at high metallicity and this result is independent from LB-1; whether it hosts or does not host a massive black hole. However, if LB-1 hosts a massive black hole we are unable to explain how such a binary star system could have formed without invoking some exotic scenarios.

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Section: Introductionmentioning

confidence: 94%

The Formation of a 70 M_⊙ Black Hole at High Metallicity

Belczyński

Hirschi

Kaiser

et al. 2020

ApJ

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“…Interestingly, we note that if the NS and BH mass spectra join to form a continuum, i.e. there is no "mass gap" between BH and NS mass distributions (as Thompson et al 2019 seem to indicate), there exists a range of values of the chirp mass M c where the nature of the binary cannot be identified uniquely based on the chirp mass only (see also Mandel et al 2015). In particular, hereafter we call "ambiguous" the chirp masses whose values are compatible with either a NSNS or a light BHNS system (see Fig.…”

Section: Introductionmentioning

confidence: 86%

Filling the Mass Gap: How Kilonova Observations Can Unveil the Nature of the Compact Object Merging with the Neutron Star

Barbieri

Salafia

Colpi

et al. 2019

ApJL

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In this letter we focus on the peculiar case of a coalescing compact-object binary whose chirp mass is compatible both with a neutron star-neutron star and black hole-neutron star system, with the black hole in the ∼ 3 − 5 M range defined as the mass gap". Some models of core-collapse supernovae predict the formation of such low-mass black holes and a recent observation seems to confirm their existence. Here we show that the nature of the companion to the neutron star can be inferred from the properties of the kilonova emission once we know the chirp mass, which is the best constrained parameter inferred from the gravitational signal in low-latency searches. In particular, we find that the kilonova in the black hole-neutron star case is far more luminous than in the neutron star-neutron star case, even when the black hole is non spinning. The difference in the kilonovae brightness arises primarily from the mass ejected during the merger. Indeed, in the considered interval of chirp masses, the mass ejection in double neutron star mergers is at its worst as the system promptly forms a black hole. Instead mass ejection for black hole-neutron star case is at its best as the neutron stars have low mass/large deformability. The kilonovae from black hole-neutron star systems can differ by two to three magnitudes. The outcome is only marginally dependent on the equation of state. The difference is above the systematics in the modeling.

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“…In addition, current observations in X-ray binaries suggest a cutoff at ∼ 5M (Özel et al 2010), while the population synthesis predicts cutoffs in both low and high mass bands (Dominik et al 2015). Very recently, a massive unseen companion with a mass of 3.3 +2.8 −0.7 M was identified in the binary system 2MASS 1 https://gracedb.ligo.org/superevents/public/O3/ J05215658+4359220 ( Thompson et al 2019), and a few MassGap candidate events (S190924h, S190930s, and S191216ap) were claimed in GraceDB. Thus, it is worth investigating both scenarios, i.e., the absence and presence of the low mass gap.…”

Section: Injection Configurationsmentioning

confidence: 98%

Black Hole Mass Function of Coalescing Neutron Star Black Hole Binary Systems: The Prospect of Reconstruction with the Gravitational Wave Observations

Tang

Wang

Wang³

et al. 2020

ApJ

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The discovery of gravitational waves from compact objects coalescence opens a brand-new window to observe the universe. With more events being detected in the future, statistical examinations would be essential to better understand the underlying astrophysical processes. In this work we investigate the prospect of measuring the mass function of black holes that are merging with the neutron stars. Applying Bayesian parameter estimation for hundreds of simulated neutron star-black hole (NSBH) mergers, we find that the parameters for most of the injected events can be well recovered. We also take a Bayesian hierarchical model to reconstruct the population properties of the masses of black holes, in the presence of a low mass gap, both the mass gap and power-law index (α) of black hole mass function can be well measured, thus we can reveal where the α is different for binary black hole (BBH) and NSBH systems. In the absence of a low mass gap, the gravitational wave data as well as the electromagnetic data can be used to pin down the nature of the merger event and then measure the mass of these very light black holes. However, as a result of the misclassification of BBH into NSBH, the measurement of α is more challenging and further dedicated efforts are needed.

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A noninteracting low-mass black hole–giant star binary system

Cited by 298 publications

References 83 publications

The Formation of a 70 M_⊙ Black Hole at High Metallicity

The Formation of a 70 M_⊙ Black Hole at High Metallicity

Filling the Mass Gap: How Kilonova Observations Can Unveil the Nature of the Compact Object Merging with the Neutron Star

Black Hole Mass Function of Coalescing Neutron Star Black Hole Binary Systems: The Prospect of Reconstruction with the Gravitational Wave Observations

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A noninteracting low-mass black hole–giant star binary system

Cited by 298 publications

References 83 publications

The Formation of a 70 M⊙ Black Hole at High Metallicity

The Formation of a 70 M⊙ Black Hole at High Metallicity

Filling the Mass Gap: How Kilonova Observations Can Unveil the Nature of the Compact Object Merging with the Neutron Star

Black Hole Mass Function of Coalescing Neutron Star Black Hole Binary Systems: The Prospect of Reconstruction with the Gravitational Wave Observations

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The Formation of a 70 M_⊙ Black Hole at High Metallicity

The Formation of a 70 M_⊙ Black Hole at High Metallicity